Typhoons in the South China Sea can whip up waves with an amplitude exceeding 20 metres.
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Typically, these waves around Jupiter have an amplitude a little higher than that of the magnetic field produced by the human brain.
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Mr. Lopez opts for an amplitude of feeling, but Mr. Neilson prefers to titillate, to tease and to flit among moods, seemingly at will.
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For one-fifth of a second, LIGO measured waves in space-time with an amplitude of 0.0000000000001 centimeters, which is millions of times smaller than an atom.
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Earthquakes are scored on a logarithmic scale of 2000 to 230, so a magnitude 2000 represents an earthquake with an amplitude 10 times greater than a magnitude 6.
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Earthquakes are scored on a logarithmic scale of 1 to 000, so a magnitude 7 represents an earthquake with an amplitude 10 times greater than a magnitude 6.
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He then uses a computer algorithm to analyse the resulting footage and determine a structure's properties, even if the vibrations recorded have an amplitude of less than a millimetre.
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After two years he produced an amplitude control device called the Hamograph, which had 12 tape loop inputs, and allowed the composer automate amplitude to shift tone and pitch and add echo.
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Crucially, if you have, say, a thousand qubits, and they can interact (to form so-called "entangled" states), the rules of quantum mechanics are unequivocal that you need an amplitude for every possible configuration of all thousand bits.
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At the correct speed of passage these waves hit a resonant frequency—increasing in amplitude as the critical speed is maintained until, at an amplitude dependent on the thickness of the sheet, that sheet will crack up and disintegrate, leaving a navigable passage behind.
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It is a suspected variable with an amplitude of about 0.05 magnitudes.
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The orbital argument of pericenter oscillates around 90° with an amplitude of 60°.
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1 Geminorum is listed as a suspected variable star with an amplitude of 0.05 magnitudes.
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Lightcurve analysis showed a concurring period of hours and an amplitude of 0.4 in magnitude ().
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In June 2018, a rotational lightcurve of Fatme was obtained from 5 nights of photometric observations by Tom Polakis at the Command Module Observatory in Arizona. Lightcurve analysis gave a rotation period of hours with a brightness variation of magnitude (). The result supersedes previously reported period determinations of hours with an amplitude of magnitude by Robert Stephens at the Santana Observatory , California, in May 2001 (), hours with an amplitude of magnitude (tentative) by French amateur astronomer Laurent Bernasconi in December 2004 (), hours with an amplitude of magnitude (tentative) by French amateur astronomer René Roy in May 2012 (), and hours with an amplitude of magnitude by the Spanish group of asteroid observers, OBAS, in January 2016 ().
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During the rise of this outburst, periodic brightness variations with an amplitude of about 0.1 magnitudes began to be seen.
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In May 1984, the object's first measurement by Richard Binzel gave a period of and an amplitude of 0.23 magnitude ().
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It has been observed to vary in brightness, but only with an amplitude of about one hundredth of a magnitude.
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Also in 2011, an ambiguous period of () with an alternative period solution of 16.10 hours and an amplitude of () magnitude was determined ().
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Brian Warner's 2015-observation supersedes a previously obtained lightcurve that gave a significantly shorter period of hours with an amplitude of 1.05 magnitude ().
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HD 118508 is a variable star in the northern constellation of Boötes. It varies marginally in luminosity with an amplitude of 0.04 in magnitude.
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Earth's net (or equivalent) equilibrium tide has an amplitude of only 3.23 cm, which is totally swamped by oceanic tides that can exceed one metre.
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In September 1992, a rotational lightcurve of Lalage was obtained from photometric observations by Polish astronomer Wiesław Wiśniewski. Lightcurve analysis gave a short rotation period of hours with a high brightness variation of magnitude, indicative of a non-spherical, elongated shape (). Since then, additional period determinations gave hours with an amplitude of magnitude () by David Higgins in October 2009, hours with an amplitude of magnitude () by Robert Stephens in January 2014, and hours with an amplitude of magnitude () by Daniel A. Klinglesmith in February 2014. A modeled lightcurves using photometric data from the BlueEye600 robotic telescope at Ondřejov Observatory gave a sidereal period of .
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The Collaborative Asteroid Lightcurve Link does not mention the asteroid's suspected binary status and consolidates a period of 4.9075 hours with an amplitude of 0.21 to 0.26.
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A second lightcurve was obtained at the Palomar Transient Factory in September 2010, and gave a concurring period of hours with an amplitude of 0.63 in magnitude ().
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Follow-up observations by Warner in February 2009 gave a concurring period of hours and an amplitude of 0.12 magnitude () with no indications of mutual occultation/eclipsing events.
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In a noise-measuring set, flat weighting is a noise weighting based on an amplitude-frequency characteristic that is flat over a frequency range that must be stated.
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Based on observations taken on September 2004, Brian Warner at his Palmer Divide Observatory , Colorado, published an ambiguous period of and hours with an amplitude of and magnitude, respectively, depending on whether the period solution is derived from a monomodal or from a bimodal lightcurve (). Alternatively, Warner also gave a revised period of hours and an amplitude of magnitude for his other observation taken on December 2000. In February 2011, James W. Brinsfield at the Via Capote Observatory in California measured a period of hours with an amplitude of magnitude (). Observations by Nicolas Esseiva and Raoul Behrend in December 2014 gave a tentative period of hours and a weak amplitude of magnitude ().
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In August 2016, the so-far best- rated rotational lightcurve of Valdivia was obtained by the Spanish amateur astronomer group OBAS. Lightcurve analysis gave a rotation period of 4.098 hours with a brightness variation of 0.25 magnitude (). Previously, in May 2003, photometric observations made by Donald P. Pray at the Carbuncle Hill Observatory near Providence, Rhode Island, gave a synodic period of 4.096 hours and an amplitude of 0.40 in magnitude (). In addition astronomers at the Palomar Transient Factory found a period of 4.096 hours with an amplitude of 0.28 om May 2011 (), and French amateur astronomer René Roy obtained a period of 8.1922 hours (twice the period solution) with an amplitude of 0.36 ().
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In March 2001, a rotational lightcurve of Colchis was obtained from photometric observations by Robert Stephens. Lightcurve analysis gave a rotation period of 23.47 hours with a brightness variation of 0.45 magnitude (). In September 2016, French amateur astronomer Patrick Sogorb measured an identical period and an amplitude of 0.46 magnitude (). A similar period of 23.41 hours with an amplitude of 0.33 magnitude was obtained by astronomers at the Palomar Transient Factory in January 2014.
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A surface acoustic wave (SAW) is an acoustic wave traveling along the surface of a material exhibiting elasticity, with an amplitude that typically decays exponentially with depth into the material.
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The General Catalogue of Variable Stars lists an amplitude of 2.7 magnitudes. Water masers have been detected around U Lacertae, common in the extended atmospheres of very luminous cool stars.
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The most recent light curve was obtained by the "Spanish Photometric Asteroid Analysis Group" (OBAS) in May 2016, which gave a period of 7.163 hours with an amplitude of 0.12 magnitude ().
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In January 2019, a rotational lightcurve of Baumeia was obtained from photometric observations by European astronomers Bruno Christmann, Raoul Behrend, Anaël Wünsche, Marc Bretton, Rui Goncalves, Josep Bosch. Lightcurve analysis gave a well-defined rotation period of hours with a brightness variation of magnitude (). The result confirms and refines previous observations by French amateur astronomer René Roy in February 2003, which gave a period of hours with an amplitude of magnitude (), by Jean-Gabriel Bosch at the French Collonges Observatory in February 2006, which gave an identical period of hours with an amplitude of magnitude (), by James W. Brinsfield at the Via Capote Observatory in Australia in November 2008, which gave the first secured period of hours with an amplitude of magnitude ().
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In October 2006, a rotational lightcurve of Burnhamia was obtained from photometric observations by Robert Buchheim at the Altimira Observatory in California. Lightcurve analysis gave a well-defined rotation period of hours with a brightness variation of magnitude (). The result supersedes previous observations by French amateur astronomer Laurent Bernasconi from May 2005, with a period of hours with an amplitude of magnitude (), and from October 2006, that gave a period of hours and an amplitude of magnitude ().
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IRC -10414 has been reported as a likely variable with a period of 768 days and an amplitude of over a magnitude. Observations of a long series of All Sky Automated Survey observations again showed variability with an amplitude over a magnitude, but with a period of 2,726 days. The variability is unlikely to be regular and the most likely classification is given as semiregular. It is not yet listed in the General Catalogue of Variable Stars.
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In March 2005, a rotational lightcurve of Begonia was obtained from photometric observations by French amateur astronomers Laurent Bernasconi, Raymond Poncy and Silvano Casulli. Lightcurve analysis gave a well-defined rotation period of hours (0.6525 days) with a brightness variation of magnitude (). An identical period of hours with an amplitude of magnitude was measured by their colleague René Roy in May 2011 (). In February 2016, Jean-Paul Godard and Frédéric Bergero also determined a period of hours and an amplitude of magnitude ().
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A rotational light curve of Delportia was obtained by American astronomer Edwin E. Sheridan in March 2007. Light curve analysis gave a well-defined rotation period of 5.615 hours with a brightness variation of 0.05 magnitude (), superseding a period of 5.5 hours with an amplitude of 0.09 magnitude obtained by French amateur astronomer René Roy in December 2005 (). In February 2010, photometric observations at the Palomar Transient Factory gave a period of 5.6204 hours and an amplitude of 0.26 magnitude ().
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In June 1981, a rotational lightcurve of Nina was obtained from photometric observations by Alan Harris at the Table Mountain and Lowell observatories. Lightcurve analysis gave a rotation period of hours with a brightness variation of magnitude (). It was confirmed by Brian Warner at his Palmer Divide Observatory in Colorado in January 2009, who determined a period of hours with an amplitude of magnitude (). In September 2012, French amateur astronomer Gérald Rousseau obtained a period of hours with an amplitude of magnitude ().
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Three other criteria for definition of the nutcracker esophagus have been defined. The Gothenburg criterion consists of the presence of peristaltic contractions, with an amplitude of 180 mm Hg at any place in the esophagus. The Richter criterion involves the presence of peristaltic contractions with an amplitude of greater than 180 mm Hg from an average of measurements taken 3 and 8 cm above the lower esophageal sphincter. It has been incorporated into a number of clinical guidelines for the evaluation of dysphagia.
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HD 158220 is a giant Be star in the southern constellation of Ara. This is a pulsating variable star that changes brightness by an amplitude of 0.030 magnitude over a period of 1.15 days.
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Photometry of CPD−57°2874 suggests that it is variable with an amplitude of perhaps 0.2 magnitudes. It has not been formally classified as a variable star and the cause of the variations is unclear.
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In January 218, a rotational lightcurve of Gutemberga was obtained from photometric observations by Tom Polakis at the Command Module Observatory in Arizona. Lightcurve analysis gave a well-defined rotation period of hours with a brightness variation of magnitude (). The result supersedes observations by Otmar Nickel of Astronomical Consortium of Mainz from February 2001, which gave a period of hours with an amplitude of magnitude (), and observations by Astronomers at the Palomar Transient Factory in California, with a period of hours and an amplitude of magnitude.().
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The result supersedes an incorrect period of hours with an amplitude of magnitude from a tentative one- night observation by French amateur astronomers Paul Krafft, Olivier Gerteis, Hubert Gully, Luc Arnold and Matthieu Bachschmidt from 2013 ().
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Slovakia has an exceptionally long rotation period of 308 hours with a high brightness variation of 1.10 magnitude (). The Collaborative Asteroid Lightcurve Link (CALL) adopts a period of 308.6 hours with an amplitude of 1.1 magnitude.
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The largest wave hit Pago Pago at 6:13 pm local time, with an amplitude of .Dunbar, Paula K. (2015). Pacific Tsunami Warning System: A Half Century of Protecting the Pacific, 1965–2015. Government Printing Office.
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The body is calculated to measure 236 meters in diameters. Its rotational period is 13.5 hours and its light curve has an amplitude of 0.9 mag which hints at a very elongated body, perhaps a contact binary.
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632 Pyrrha is a minor planet orbiting the Sun. Photometric observations of the minor planet in 2011 gave a rotation period of with an amplitude of in magnitude. This result rules out previous determinations of the period.
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Over four nights in January 2013, a rotational lightcurve of Subamara was obtained from photometric observations by Michael Alkema at the Elephant Head Observatory in Arizona. Lightcurve analysis gave a well-defined rotation period of hours with a brightness variation of magnitude (). James Folberth and colleges of the Rose-Hulman Institute of Technology previously observed this asteroid at Oakley Southern Sky Observatory in August 2011, finding a period of hours with an amplitude of magnitude (). In November 2017, Tom Polakis at the Command Module Observatory in Tempe, Arizona, determined hours with an amplitude of magnitude ().
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The electronics theory indicated that a frequency modulated signal would have infinite bandwidth; for an amplitude modulated signal, the bandwidth is approximately twice the highest modulating frequency. Armstrong realized that while a frequency modulated signal would have an infinite bandwidth, only the first few sets of sidebands would be significant; the rest could be ignored.The ARRL Handbook for Radio Communication, American Radio Relay League, 2008, p. 9.30 An amplitude modulated voice channel bandwidth would be approximately 6 kilohertz; a common frequency modulated voice channel bandwidth could be 15 kilohertz.
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In the theory of quantum communication, an amplitude damping channel is a quantum channel that models physical processes such as spontaneous emission. A natural process by which this channel can occur is a spin chain through which a number of spin states, coupled by a time independent Hamiltonian, can be used to send a quantum state from one location to another. The resulting quantum channel ends up being identical to an amplitude damping channel, for which the quantum capacity, the classical capacity and the entanglement assisted classical capacity of the quantum channel can be evaluated.
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In January 2017, a rotational lightcurve of Pickeringia was obtained from photometric observations by the Spanish group of asteroids observers (OBAS). Lightcurve analysis gave a rotation period of hours with a brightness variation of magnitude (). The result supersedes observations taken during the 1990s by European astronomers using the ESO 0.5-metre telescope at La Silla Observatory, Chile, which gave a period of hours with an amplitude of magnitude (). as well as a period determination by French amateur astronomer Laurent Bernasconi in December 2004, which gave and an amplitude of magnitude ().
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In March 2015, a rotational lightcurve of Bredichina was obtained from photometric observations by Spanish astronomers Alfonso Carreño , Amadeo Aznar , Enrique Arce , Pedro Brines , and Juan Lozano . Lightcurve analysis gave a rotation period of hours with a brightness variation of magnitude (). Previously, in August 2008, Argentine astronomer Ricardo Gil-Hutton derived period of hours with an amplitude of magnitude (). Tentative measurements were also made by Italian Nicola Cornero and Federico Manzini at the Sozzago Astronomical Station in May 2010, which gave a period of hours with an amplitude of magnitude ().
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GP Andromedae (often abbreviated to GP And) is a Delta Scuti variable star in the constellation Andromeda. It is a pulsating star, with its brightness varying with an amplitude of 0.55 magnitudes around a mean magnitude of 10.7.
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The star varies in brightness by an amplitude of 0.0156 in magnitude over a period of 26 days. The effective temperature of the outer atmosphere is 3,839 K, giving it the ruddy hue of an M-type star.
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The theory of superfluid transitions in two dimensions is known as the Kosterlitz-Thouless (KT) theory. The 2D XY model - where the order parameter is characterized by an amplitude and a phase - is the universality class for this transition.
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It is a candidate variable star of unknown type, showing an amplitude variation of 0.0115 magnitude with a frequency of 0.47645 times per day, or one cycle per 2.1 days. X-ray emission has been detected from this system.
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Recent calculations indicate that it is a stable Mars Trojan candidate with a libration period of 1400 yr and an amplitude of 18°. values as well as its short-term orbital evolution are similar to those of 5261 Eureka.
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The phase noise becomes important when the energy of the frequency modulation or phase modulation of waves is comparable to the energy of the signal (which is believed to be more robust with respect to additive noise than an amplitude modulation).
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1a) is transferred to a phase squeezed state (Fig. 1b) or to an amplitude squeezed state (Fig. 1c), depending on the relative phase between coherent input field and pump field. A graphical description of these processes can be found in.
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In May 2015 a collaboration of Spanish amateur astronomers including Alfonso Garceràn , Amadeo Macias , Enrique Mansego , Pedro Rodriguez and Juan de Haro measured a period of hours—or half the period solution of the other observations, with an amplitude of magnitude ().
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Two more lightcurves were obtained by Brian Warner at this Palmer Divide Observatory in Colorado, United States, in August 2004 and August 2010, who measured a period of 4.930 and 5.28 hours with an amplitude of 0.11 and 0.14 magnitude, respectively.
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Recent calculations indicate that it is a stable Mars trojan asteroid with a libration period of 1350 yr and an amplitude of 14°. These values as well as its short-term orbital evolution are similar to those of 5261 Eureka or .
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Associated with propagation of a disturbance are several different velocities. For definiteness, consider an amplitude modulated electromagnetic carrier wave. The phase velocity is the speed of the underlying carrier wave. The group velocity is the speed of the modulation or envelope.
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In November 2005, a rotational lightcurve of Seraphina was obtained from photometric observations by French amateur astronomer Raymond Poncy. Lightcurve analysis gave a rotation period of hours with a low brightness variation of magnitude, indicative of a rather spherical shape (). Other observations include a period of hours with an amplitude of magnitude by Richard Binzel from June 1984 (), and a period of hours with an amplitude of magnitude by the Spanish group of asteroid observers, OBAS, in November 2015 (). In 2018, Czech astronomers Josef Ďurech and Josef Hanuš published a modeled lightcurve using photometric data from the Gaia spacecraft's second data release.
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Several high-quality rotational lightcurves were obtained from photometric observations since 2003. An observation by Brian Warner at the U.S. Palmer Divide Observatory in Colorado rendered a rotation period of hours with a high brightness variation of 0.67 in magnitude (), indicating that the body has a non-spherical shape. This observation concurs with another measurement taken at the Oakley Observatory that rendered a period of and an amplitude of 0.50 mag (), superseding a less accurate lightcurve produced by the PDS of 8.40 hours (). In 2011, an observation by René Roy gave another concurring period of hours and an amplitude of 0.79 mag ().
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In December 2010, a rotational lightcurve of Deipylos was obtained from photometric observations in the R-band by astronomers at the Palomar Transient Factory in California. Lightcurve analysis gave a rotation period of 11.490 hours with a brightness amplitude of 0.11 magnitude () Between 2015 and 2017, several observations by Robert Stephens in collaboration with Daniel Coley and Brian Warner at the Center for Solar System Studies in California gave a more refined period between 9.19 and 9.38 hours and an amplitude of 0.07–0.13 magnitude (). The best-rated result gave 9.298 hours with an amplitude of magnitude.
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A comparison between AAM and LOD shows that they are highly correlated. In particular, one recognizes an annual period of LOD with an amplitude of 0.34 milliseconds, maximizing on February 3, and a semiannual period with an amplitude of 0.29 milliseconds, maximizing on May 8, as well as 10‑day fluctuations of the order of 0.1 milliseconds. Interseasonal fluctuations reflecting El Niño events and quasi-biennial oscillations have also been observed. There is now general agreement that most of the changes in LOD on time scales from weeks to a few years are excited by changes in AAM.
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In September 2000, a rotational lightcurve of Hirundo was obtained from photometric observations by American Brian Warner at the Palmer Divide Observatory in Colorado. Lightcurve analysis gave a rotation period of hours with a high brightness variation of magnitude, indicative of an elongated shape (). During the same opposition, Bill Holliday measures a period of () and an amplitude of () magnitude at his River Oaks Observatory in New Braunfels, Texas (). Further observations by René Roy (2011), Patrice Le Guen (2018), and Anaël Wünsche and Raoul Behrend (2020) determined a period of (), () and () with an amplitude of (), () and () magnitude, respectively ().
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In August 2013, a rotational lightcurve of Hagar was obtained from nine nights of photometric observations by Frederick Pilcher at the Organ Mesa Observatory in Arizona. Analysis gave a well- defined, classically shaped bimodal lightcurve with a rotation period of () hours and a high brightness variation of magnitude (). At the same time, Alexander Kurtenkov at Sofia University, Bulgaria, obtained a concurring period of hours with an amplitude of magnitude (). In July 2017, French and Swiss astronomers René Roy and Raoul Behrend confirmed the period measuring a nearly identical rotation of () hours and an amplitude of magnitude ().
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For an amplitude-squeezed state, the most narrow distribution of the wave packet is reached at the field maximum, resulting in an amplitude that is defined more precisely than the one of a coherent state. For a phase-squeezed state, the most narrow distribution is reached at field zero, resulting in an average phase value that is better defined than the one of a coherent state. In phase space, quantum mechanical uncertainties can be depicted by the Wigner quasi-probability distribution. The intensity of the light wave, its coherent excitation, is given by the displacement of the Wigner distribution from the origin.
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A basically identical period of hours with a brightness variation of magnitude was determined by French amateur astronomer René Roy in February 2011 (). In March 2016, the Spanish group of asteroid observers, OBAS, measures a period of hours with an amplitude of magnitude ().
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DS Crucis is a variable star with an amplitude of about 0.05 magnitudes. It was found to be variable from the photometry performed by the Hipparcos satellite. The variability type is unclear but it is assumed to be an α Cygni variable.
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There are three important properties of a hologram which are defined in this section. A given hologram will have one or other of each of these three properties, e.g. an amplitude modulated, thin, transmission hologram, or a phase modulated, volume, reflection hologram.
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In January 2013, a rotational lightcurve of Graun was obtained from photometric observations. Lightcurve analysis gave a rotation period of hours with a brightness variation of 0.16 magnitude (). The measurement supersedes a shorter period of 20 hours with an amplitude of 0.2 magnitude ().
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Photometry from the Hipparcos satellite mission showed that DU Crucis varies in brightness with an amplitude of 0.44 magnitudes. No periodicity could be detected in the variations and it was classified as a slow irregular variable of type Lc, indicating a supergiant.
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It varies slightly in brightness, with a periodicity of 6.2 days and an amplitude change of 0.0096 in magnitude. On average it is radiating 387 times the luminosity of the Sun from its enlarged photosphere at an effective temperature of 4,013 K.
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To measure or display the modulating waveform of a modulated high-frequency signal—for example, an amplitude-modulated radio signal—a probe fitted with a simple diode demodulator can be used. The probe will output the modulating waveform without the high-frequency carrier.
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It has a likely period of 0.22132 days and is thought to be a β Cephei variable or slowly pulsating B-type star. Hipparcos photometry shows an amplitude of 0.035 magnitudes. It has a rotational velocity of 275 km/s, one of the highest known.
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The first tourist accommodation, the Hotel Eureka was built in 1933. At present the town has 61 hotels and about 65 self-catering apartments. The beach at Cala Millor is 1.8 kilometres long. On average it has got an amplitude of 30m to 35m.
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A concurring period of 37.6083 hours with an amplitude of 0.19 magnitude was measured by astronomers at the Palomar Transient Factory in October 2013 (). While not being a slow rotator, its period is significantly longer than that of most larger Jupiter trojans (see list below).
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An ambiguous lightcurve was obtained through photometric observations by Czech astronomer Petr Pravec in 1998. The light-curve gave a rotation period of hours with a brightness amplitude of 0.20 in magnitude. The alternative period solution is hours with an amplitude of 0.22 in magnitude ().
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It gave a period of 2.978 hours and an amplitude of 0.25 magnitude (). In 2016, an international study modeled a lightcurve with a concurring period of 2.978301 hours and found a spin axis of (277.0°, 57.0°) and (66.0°, 48.0°) in ecliptic coordinates (λ, β) ().
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In June 2016, a rotational lightcurve of Demeter was obtained from photometric observations by American astronomers Tom Polakis and Brian Skiff at the Command Module Observatory in Tempe, Arizona. Lightcurve analysis gave a rotation period of 9.846 hours with an amplitude of 0.12 magnitude (). Observations by the Spanish OBAS group, also taken during the 2016-opposition, gave a concurring period of 9.870 hours and a brightness variation of 0.11 magnitude (). The results supersede previous observations by Robert Stephens, Olivier Thizy, René Roy and Stéphane Charbonnel from July 2001, which gave a period of 9.70 and 9.701 hours with an amplitude of 0.12 and 0.14 magnitude, respectively.
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In October 2013, a rotational lightcurve of Benda was obtained from photometric observations over two nights by Robert Stephens at the Center for Solar System Studies in California. Lightcurve analysis gave a well-defined rotation period of hours with a brightness variation of magnitude (). In August 1995, a first period of hours was determined by Stefano Mottola (). In March 2004, French amateur astronomer René Roy obtained a period of hours with an amplitude of magnitude from three nights of observations (), while Robert K. Buchheim determined a period of hours and an amplitude of magnitude observing Benda over 10 nights at the Altimira Observatory in November 2007 ().
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At point 0 along the fiber, the wave in polarization mode 1 induces an amplitude into mode 2 at some phase. However at point 1/2 Lb along the fiber, the same coupling coefficient between the polarization modes induces an amplitude into mode 2 which is now 180 degrees out of phase with the wave coupled at point zero, leading to cancellation. At point Lb along the fiber the coupling is again in the original phase, but at 3/2 Lb it is again out of phase and so on. The possibility of coherent addition of wave amplitudes through crosstalk over distances much larger than Lb is thus eliminated.
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In preparation for the planned visit by the Lucy spacecraft, Leucus was once again observed by astronomers Marc Buie at SwRI and Stefano Mottola at DLR in 2016. The obtained bimodal lightcurve gave a somewhat shorter period of 440 hours and an amplitude of 0.7 magnitude.
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The vertical dimension of a fold can be described as an amplitude. The horizontal dimension of a fold can by described by wavelength and hinge line of a fold. As a fold grows in three- dimension, amplitude, wavelength and the length of the hinge line will increase.
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In 2018, however, an international photometric survey, using archived photometric data from the Geneva Observatory as well from dedicated observations, modeled a far longer period of hours with an amplitude of magnitude (). The survey uses combines convex lightcurve inversion with a non-convex algorithm (SAGE) to derive their periods.
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Stars in this class are type Bp supergiants with a period of 0.1–1 day and an amplitude of 0.1 magnitude on average. Their spectra are peculiar by having weak hydrogen while on the other hand carbon and helium lines are extra strong, a type of Extreme helium star.
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In October 2011, a rotational lightcurve of Simeïsa was obtained from photometric observations by French amateur astronomer René Roy. Lightcurve analysis gave a rotation period of () hours with a brightness variation of () magnitude (). In the 1990s, Mats Dahlgren already determined a period of hours with an amplitude of magnitude ().
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For example, a Morse code transmitter combines source coding, channel coding, and line coding into one step, typically followed by an amplitude modulation step. Barcodes, on the other hand, add a checksum digit during channel coding, then translate each digit into a barcode symbol during line coding, omitting modulation.
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During five nights in December 2017, a rotational lightcurve of Angelica was obtained from photometric observations by Tom Polakis at the Command Module Observatory in Tempe, Arizona. Lightcurve analysis gave a rotation period of hours with a very low brightness variation of magnitude (), which is indicative of regular, spherical shape. Another observation from January 2018, by Brigitte Montminy and Katherine McDonald at Minnetonka High School, and Russell Durkee at the Shed of Science Observatory in Minnetonka, Minnesota, determined a concurring period of hours with an amplitude of magnitude (). Federico Manzini at the Sozzago Astronomical Station obtained the object's first lightcurve in December 2006, measuring a period of hours and an amplitude magnitude ().
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In November 2000, photometric observations by Brian Warner at the Palmer Divide Observatory () in Colorado Springs, Colorado, were used to build a lightcurve for Utopia. The asteroid displayed a rotation period of 13.61 hours and a brightness variation of 0.28 magnitude, revised from a previous publication that gave 13.60 hours and an amplitude of 0.29 (). In September 2005, French amateur astronomers Laurent Bernasconi, Raymond Poncy and Pierre Antonini obtained a lightcurve with a concurring period of 13.623 hours and an amplitude of 0.36 magnitude (). In 2011, a modeled lightcurve using data from the Uppsala Asteroid Photometric Catalogue (UAPC) and other sources gave a sidereal period 13.6228 hours, as well as a fragmentary spin axis of (n.a.
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Based upon photometry observations between 1984−2007, it has a sidereal rotation period of 8.283065 h with an amplitude that can range up to in magnitude. The lightcurve shows some shape irregularities. There are two valid solutions for the pole's ecliptic coordinates: (λ1, β1) = (38°, +75°) and (λ2, β2) = (237°, +73°).
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Three possible occultation events were observed, suggesting that Parchomenko might be a binary asteroid, having a minor-planet moon as companion. However, no new findings have been made since. In October 2008, Italian amateur astronomer Silvano Casulli measured a similar period of 3.08 hours with an amplitude of 0.27 magnitude ().
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14 Aquarii (abbreviated 14 Aqr) is red giant star. 14 Aquarii is the Flamsteed designation; it also bears the variable star designation IW Aquarii. It is a semiregular variable with an amplitude of less than a tenth of a magnitude, and shows variations on a timescale of just one day.
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This is a periodic variable of unknown type, changing in brightness with an amplitude of 0.0161 magnitude at a frequency of 0.23354 d−1, or once every 4.3 days. The third component is a magnitude 13.0 star at an angular separation of along a position angle of 164°, as of 2015.
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The pressure applied to the abrasive is very light, usually between , but can be as high as . Honing is usually and grinding is between . When a stone is used it is oscillated at 200 to 1000 cycles with an amplitude of . Superfinishing can give a surface finish of 0.01 μm.
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This is a variable star most likely of the RS CVn type with an amplitude of 0.15 in magnitude, and it displays magnetic activity. It has 5.25 times the mass of the Sun and, having exhausted the supply of hydrogen at its core, has expanded to 38 times the Sun's radius.
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The Pas experiences a humid continental climate (Köppen Dfb) with long cold winters and short warm summers. The seasonal temperature range is between , resulting in an amplitude of . The highest temperature ever recorded in The Pas was on 19 July 1941. The coldest temperature ever recorded was on 18 February 1966.
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In September 2008, a rotational lightcurve of ' was obtained from photometric observations. Lightcurve analysis gave a rotation period of hours with a brightness variation of 0.33 magnitude (). Observations by Stefano Mottola at the Calar Alto Observatory in October 2009 showed a divergent period of 7.631 hours with an amplitude of 0.20 magnitude ().
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Photometric observations of the minor planet in 2011 gave a rotation period of with an amplitude of in magnitude. This result is consistent with previous determinations. Two stellar occultation events involving this asteroid were observed from multiple sites in 2009. The resulting chords matched a smooth elliptical cross-section with dimensions of × .
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Isobes binary nature still needs further observations. Isobe was also observed by American astronomer Robert Stephens at the Center for Solar System Studies in September 2015, giving a period of 4.241 hours with an amplitude of 0.22 magnitude. However, no mutual occulation events have been found during the two-night long observation period ().
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The event was visible from Australia and New Zealand. The asteroid has been observed in 3 more stellar occultation events. Photometric observations of this asteroid in 2016 produced lightcurves indicating a rotation period of 9.9 hours with an amplitude variation of 0.18 in magnitude. This result matched previous determinations of the spin rate.
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In October 2012, a rotational lightcurve of Kirkwood was obtained from photometric observations at the Etscorn Campus Observatory () in New Mexico, United States. Lightcurve analysis gave a rotation period of 12.518 hours with a brightness variation of 0.05 magnitude (). Another lightcurve gave a period of 17.9 hours and an amplitude of 0.22 magnitude ().
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The lightcurve study also showed that Grahamchapman itself has a rotation period of 2.28561 hours with a brightness variation of 0.10 magnitude (). A second photometric observation in December 2008, gave an identical period with an amplitude of 0.11 magnitude (). A low brightness amplitude typically indicates that the body has a nearly spheroidal shape.
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A grid leak resistor and capacitor unit from 1926. The 2 megohm cartridge resistor is replaceable so the user can try different values. The parallel capacitor is built into the holder. A grid leak detector is an electronic circuit that demodulates an amplitude modulated alternating current and amplifies the recovered modulating voltage.
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In May 1984, American astronomer Richard Binzel obtained a rotational lightcurve of Geneviève that gave a rotation period of 16.37 hours with a brightness variation of 0.23 magnitude (). A divergent period of 24.82 hours with an amplitude of 0.07 magnitude was obtained from photometric observations by astronomer Raymond Poncy in April 2005 ().
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Lightcurve-based 3D-model of Tanina In February 2002, a rotational lightcurve of Tanina was obtained from photometric observations by Italian astronomer Andrea Ferrero at the Bigmuskie Observatory . Lightcurve analysis gave a well-defined rotation period of hours with a high brightness variation of magnitude, indicative of an elongated, non-spherical shape (). The result supersedes previous period determinations of hours with an amplitude of magnitude () by Wiesław Z. Wiśniewski from February 1992, and hours with an amplitude of magnitude () by Agnieszka Kryszczyńska in May 1999. In 2011, a modeled lightcurve using data from the Uppsala Asteroid Photometric Catalogue (UAPC) and other sources gave a sidereal period hours, as well as two spin axes at (46.0°, 48.0°) and (231.0°, 60.0°) in ecliptic coordinates (λ, β).
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In November 2004, a rotational lightcurve of Jose was obtained from photometric observations by amateur astronomers Rui Goncalves and Laurent Bernasconi in Portugal and France, respectively. Lightcurve analysis gave a well-defined rotation period of hours and a brightness variation of 0.68 magnitude (), indicative of a non-spherical, elongated shape. During an extensive lightcurve survey of Koronian asteroids by visiting American astronomers using the 0.6-m telescope at Mauna Kea Observatory of the Institute for Astronomy in Hawaii during 1997–2005, another period of with an amplitude of 0.80 magnitude was determined (). French amateur astronomer René Roy and the team at the Palomar Transient Factory in California also measured as period of and with an amplitude of 0.82 and 0.96, respectively ().
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The first rotational lightcurves of Antenor were obtained from photometric observations in October 1989, by astronomers Mario Di Martino and Maria Gonano–Beurer with the now decommissioned ESO 1-metre telescope at La Silla in Chile. In April 1969, a follow-up observation by Mottola gave the so-far best-rated rotation period of in 7.965 hours with a brightness variation of 0.09 magnitude (). In September 2012, by astronomers at the Palomar Transient Factory derived two concurring period of hours with an amplitude of 0.12 and 0.15 in the R- and S-band respectively (). Between 2016 and 2018, observation by Robert Stephens at the Center for Solar System Studies, California, gave rotation period of 7.906, 7.964 hours with an amplitude of 0.09 ().
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In May 1991, observations by Stefano Mottola using the now decommissioned ESO 1-metre telescope at ESO's La Silla Observatory in Chile gave a rotation period of 9.838 hours at an amplitude of 0.24 magnitude (). Follow-up observations were made in 1992 and 2009 – in order to rule out any alternative period solutions, as the irregular lightcurve showed additional maxima and minima – gave a concurring period of 9.840 hours with a brightness variation of 0.31 magnitude (). In April 2014, another rotational lightcurve was obtained by Robert Stephens and Daniel Coley at the Center for Solar System Studies in California in collaboration with Linda French from Illinois Wesleyan University. Lightcurve analysis gave a well-defined rotation period of 9.818 hours with an amplitude of 0.27 magnitude ().
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Three rotational lightcurves of Automedon have been obtained from photometric observations, that are all in good agreement. In June 1994, observations by Stefano Mottola using the now decommissioned Bochum 0.61-metre Telescope at ESO's La Silla Observatory in Chile gave a rotation period of 10.220 hours with a brightness variation of 0.12 magnitude (). A second lightcurve gave a period of 10.212 hours with an amplitude of 0.17 magnitude. It was measured in July 2007, by astronomers using telescopes at the Calvin College Observatory in Michigan and the Calvin- Rehoboth Robotic Observatory in New Mexico (). In June 2017, another observation by Brian Warner and Robert Stephens at the Center for Solar System Studies in California gave a period of 10.223 hours with an amplitude of 0.11 magnitude ().
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Several rotational lightcurves for this asteroid were obtained from photometric observations. In December 2004, the first lightcurve by American astronomer Brian Warner at his Palmer Divide Observatory (PDS) in Colorado, gave a rotation period of hours with a brightness variation of in magnitude (). Between 2008 and 2012, three additional lightcurves at the PDS gave an almost identical period of 5.485 hours with an amplitude of 0.67, 0.74 and 1.02, respectively (). Other lightcurves were obtained by Hanuš at the French CNES and other institutions, which gave a period of hours (), and by Italian astronomer Federico Manzini at SAS observatory in Novara, Jean Strajnic and Raoul Behrend from December 2012, which rendered a period of hours with an amplitude of 0.66 in magnitude ().
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In November 2008, a rotational lightcurve of Herluga was obtained from photometric observations by James W. Brinsfield at the Via Capote Observatory in California. Lightcurve analysis gave a rotation period of hours with a brightness variation of magnitude (). In August 2016, an alternative period determination of hours with an amplitude of mag was published ().
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Ampliphase is the brand name of an amplitude modulation system achieved by summing phase modulated carriers. This modulation and amplifier technology family was originally marketed by RCA for AM broadcast transmitters. The Ampliphase system was not developed by RCA, but by McClatchy Broadcasting in the mid-1930s. McClatchy Broadcasting acquired the technology via patent acquisition.
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It is a suspected rotating ellipsoidal variable with a period of 0.64 days and an amplitude of 0.07 magnitude. Confirmation would indicate that this is a close binary system. It has an estimated age of around 57 million years. In Chinese, (), meaning Son, refers to an asterism consisting of λ Columbae and β Columbae.
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In August 2015, two rotational lightcurves of Amphimachus were obtained from photometric observations by the Kepler space observatory. Best-rated lightcurve analysis by Gyula M. Szabó gave a rotation period of hours with a brightness amplitude of 0.22 magnitude (). The second, concurring observation gave a period of 8.39 hours and an amplitude of 0.20 magnitude ().
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In February 2011, a rotational lightcurve of Chaliubieju was obtained French amateur astronomer Pierre Antonini. Lightcurve analysis gave a rotation period of 3.986 hours with a brightness variation of 0.27 magnitude (). One month later another photometric observation at the Astronomical Research Observatory () gave a concurring period of 3.984 hours and an amplitude of 0.30 magnitude ().
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In November 2007, a rotational lightcurve, constructed from photometric observations by Crag Bennefeld at the Rick Observatory, gave a rotation period of hours with a brightness variation of 0.23 in magnitude (). Another lightcurve, obtained by French astronomers Pierre Antonini and René Roy in February 2013, gave a period of hours with an amplitude of 0.18 ().
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Rafitas first rotational lightcurve was obtained by American astronomer Alan Harris of JPL in January 1981. It gave a rotation period of 5.100 hours with a brightness variation of 0.31 magnitude (). Photometric observations by French amateur astronomer Laurent Bernasconi in December 2004, gave a period of 6.800 hours and an amplitude of 0.13 magnitude ().
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Several rotational lightcurves of Kniertje have been obtained from photometric observations since 2003. Lightcurve analysis gave a rotation period between 9.78 and 9.872 hours with a brightness variation between 0.15 and 0.32 magnitude (). An alternative period solution of 12.255 hours with an amplitude of 0.33 magnitude was found by Brian Warner in March 2006 ().
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Radio emission was detected from this system in 1985/86. The supergiant primary is a slow irregular variable with an amplitude of about 0.1 magnitudes. Its close companion has 57% of the mass of the Sun. The secondary is a hot B-type main-sequence star, but still 2.5 magnitudes fainter than the primary.
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On 15 July 2013, the album cover artwork was revealed. On 2 September 2013, Arctic Monkeys revealed a track titled "I Want It All" during a XFM radio show, and exclusively played "One for the Road" on Zane Lowe's BBC Radio 1 show. The waveform depicted is characteristic of an amplitude modulated (AM) signal.
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In January 2006, a rotational lightcurve of Tripaxeptalis was obtained from photometric observations by astronomer Adrián Galád at Modra Observatory in Slovakia. Lightcurve analysis gave a rotation period of 2.33 hours with a brightness variation of 0.10 magnitude (). The ambiguous lightcurve gave an alternative period solution of 2.23 hours and an amplitude of 0.10.
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An amplitude splitting interferometer uses a partial reflector to divide the amplitude of the incident wave into separate beams which are separated and recombined. Fig. 6 illustrates the Fizeau, Mach–Zehnder and Fabry–Pérot interferometers. Other examples of amplitude splitting interferometer include the Michelson, Twyman–Green, Laser Unequal Path, and Linnik interferometer. Figure 6.
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In December 1999, a rotational lightcurve of Massinga was obtained from photometric observations by Robert A. Koff at his observatory in Colorado. Lightcurve analysis gave a rotation period of hours with a brightness variation of magnitude (). In March 2006, Laurent Bernasconi and Rui Goncalves determined a similar period of hours and an amplitude of magnitude ().
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They have the spectrum of a B-type main sequence star with a stellar classification of B5 V. The luminosity has a micro-variability with a frequency of 0.94483 cycles per day and an amplitude of 0.0067 in magnitude. The third component is a magnitude 10 star at an angular separation of 0.51 arc seconds.
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HD 105382 (also known as V863 Centauri) is a star in the constellation Centaurus. Its apparent magnitude is 4.47. From parallax measurements, it is located 130 parsecs (440 light years) from the sun. HD 105382 is a variable star whose apparent magnitude varies with an amplitude of 0.012 over a period of 1.295 days.
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Frederique Constant escapement made of silicon; anker, wheel and plateau In April 2008, Frederique Constant created a tourbillon with a silicon escape-wheel and, for the first time, an amplitude of over 300 degrees between its vertical and horizontal positions. Coupled with rapid oscillation, this gives the watch an unusually high level of precision.
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The star appears to be a Beta Cephei variable with a pulsation period of 0.0919 days and an amplitude of 0.0080 in magnitude. The magnitude 5.39 secondary, component B, is classified as a Gamma Cassiopeiae type variable star. Due to its variable nature, the brightness of the system varies from magnitude +4.42 to +4.82.
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Photometric observations of this asteroid at the Rozhen Observatory in Bulgaria during 2010 gave a light curve with a period of 4.7992 hours and a brightness variation of Δm=0.22 mag. This is consistent with a period of 4.804 hours and an amplitude of 0.24 obtained during a 1977 study. It has a cross- sectional size of .
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The spectrum of 89 Julia shows the signature of silicate rich minerals with possible indications of an abundant calcic clinopyroxene component. It is classified as an S-type asteroid. The asteroid has an estimated diameter of . Photometry from the Oakley Observatory during 2006 produced a lightcurve that indicated a sidereal rotation period of with an amplitude of in magnitude.
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Two rotational lightcurve of Alschmitt obtained in 2003 and 2004, by René Roy and Laurent Bernasconi, gave a well-defined rotation period of 7.0613 and 7.062 hours with a brightness variation of 0.39 and 0.52 in magnitude, respectively (). In October 2010, the Palomar Transient Factory derived a period of 7.0602 hours with an amplitude 0.49 magnitude ().
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In December 2010, a rotational lightcurve of Bechuana was obtained from photometric observations by astronomers at the Palomar Transient Factory in California. Lightcurve analysis gave a rotation period of 15.681 hours with a brightness variation of 0.29 magnitude (). In January 2011, astronomers Pierre Antonini and Silvano Casulli measured a refined period of 15.692 hours with an amplitude of 0.30 ().
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In January 2007, a rotational lightcurve obtained by Italian amateur astronomer Antonio Vagnozzi gave a well-defined rotation period of 3.01555 hours with a brightness variation of 0.11 magnitude (). In Spring 2014, photometry at the Palomar Transient Factory in California gave two lightcurves with a period of 3.016 and 3.02 hours and an amplitude of 0.12 magnitude ().
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In 2012, a rotational lightcurve of Palazzolo was obtained from photometric observations at the Palomar Transient Factory in California. Lightcurve analysis gave a rotation period of hours with a brightness amplitude of 0.16 in magnitude (). Follow-up observations in 2013 and 2014, gave a similar period of and hours with an amplitude of 0.16 and 0.14, respectively ().
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Two rotational lightcurves of Lugano were obtained from photometric observations made in February 2005. The first lightcurve by French astronomer Raymond Poncy gave a rotation period of hours with a brightness variation of 0.25 magnitude (). The second lightcurve from the U.S. Carbuncle Hill Observatory (), Rhode Island, rendered a well-defined period of with an amplitude of 0.31 in magnitude ().
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In April 2006, photometric observations of Luu collected by American astronomer Brian D. Warner at his Palmer Divide Station, Colorado, show a rotation period of hours with a brightness variation of magnitude (). A second, tentative lightcurve was obtained by French astronomer René Roy in July 2007. It gave a period of hours and an amplitude of 0.05 in magnitude ().
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In April 2004, a rotational lightcurve of Milankovitch was obtained from photometric observations by American amateur astronomer Walter R. Cooney Jr.. It gave a rotation period of hours with a brightness variation of 0.12 magnitude (). In October 2006, French astronomer Pierre Antonini obtained another lightcurve, which gave a similar period of and an amplitude of 0.14 magnitude ().
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American astronomer Richard Binzel obtained the first rotational lightcurve of Rosseland in the early 1980s. It gave a rotation period of 69.2 hours with a brightness variation of 0.13 magnitude (). During a survey of presumed slow rotators, photometric observations by Brazilian Cláudia Angeli and colleges gave a period of 69.2 hours and an amplitude of 0.45 magnitude ().
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The information can be added to the carrier in several different ways, in different types of transmitters. In an amplitude modulation (AM) transmitter, the information is added to the radio signal by varying its amplitude. In a frequency modulation (FM) transmitter, it is added by varying the radio signal's frequency slightly. Many other types of modulation are also used.
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It is a suspected variable star, with an amplitude of 0.012 magnitude and period 4.4 days. The star has 1.3 times the mass of the Sun and has expanded to nearly 52 times the Sun's radius. It is radiating 551 times the luminosity of the Sun from its enlarged photosphere at an effective temperature of 4,000 K.
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In July 1984, a first rotational lightcurve of Lunaria was obtained by American astronomer Richard Binzel. Lightcurve analysis gave a rotation period of 7.74 hours with a brightness variation of 0.13 magnitude (). In September 2004, Donald Pray at the Carbuncle Hill Observatory () derived a refined period of 6.057 hours with an amplitude of 0.27 magnitude from photometric observations ().
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It has a well determined rotation period of hours with a brightness amplitude of 0.30 in magnitude (). Between 2011 and 2013, three additional lightcurves with concurring periods of McMath with an amplitude between 0.32 and 0.39 magnitude were obtained through photometric observations in the R- and S-band at the U.S. Palomar Transient Factory in California ().
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The asteroid has an ambiguous rotation period. A lightcurve of Mercedes obtained in 1998, gave a period of 6.448 hours and a brightness variation of 0.10 magnitude (), while another lightcurve from 2007, gave a much longer period of 24.64 hours with an amplitude of 0.15 (). A third period of 15.6 hours is considered of poor quality ().
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In October 2003, a rotational lightcurve of Imprinetta was obtained from photometric observations by American John Menke at his observatory in Barnesville, Maryland. Lightcurve analysis gave a well-defined rotation period of 8.107 hours with a brightness variation of 0.20 magnitude (). An alternative observation gave a lightcurve with period of 7.9374 hours and an amplitude of 0.20 magnitude ().
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In February 2004, a rotational lightcurve of Cambridge was obtained from photometric observations by French amateur astronomer René Roy. Lightcurve analysis gave a rotation period of 8.80 hours with a brightness variation of 0.21 magnitude (). In October 2010, observations at the Palomar Transient Factory, California, gave a longer period of 12.200 hours with an amplitude of 0.20 magnitude ().
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In July 2007, a rotational lightcurve of Vitja was obtained from photometric observations by French amateur astronomer René Roy. Lightcurve analysis gave a rotation period of 5.7014 hours and a brightness variation of 0.18 magnitude (). Another observation by Andrea Ferrero at the Bigmuskie Observatory in Italy showed a period of 6.332 with an amplitude of 0.21 ().
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Seismic surface waves travel along the Earth's surface. They can be classified as a form of mechanical surface waves. They are called surface waves, as they diminish as they get further from the surface. They travel more slowly than seismic body waves (P and S). In large earthquakes, surface waves can have an amplitude of several centimeters.
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In September 2008, a rotational lightcurve was obtained from photometric observations made by Italian astronomer Federico Manzini at the Stazione Astronomica di Sozzago (), Italy. It rendered it a rotation period of hours with a brightness variation of 0.13 in magnitude (). Previously, a fragmentary lightcurve from the 1990s, gave a shorter period of 7.1 hours with an amplitude of 0.25 ().
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In 2006, a rotational lightcurve of Abt was obtained from photometric observation at Hunters Hill Observatory, Australia. Lightcurve analysis gave a well-defined rotation period of hours with a brightness variation of 0.30 magnitude (). In 2012, a second lightcurve from the Palomar Transient Factory, California, gave a concurring period of hours with an amplitude of 0.33 magnitude ().
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The interferometry- measured angular diameter of this star is , which, at its estimated distance, equates to a physical radius of about 137 times the radius of the Sun. It is classified as a semi-regular variable star and its brightness varies by an amplitude of 0.0636 in magnitude. The identified pulsation periods are 32.3, 38.5, and 44.9 days.
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A rotational lightcurve was obtained based on photometric observations at the Australian Oakley Southern Sky Observatory in August 2012. The lightcurve showed a period of hours with a brightness amplitude of 0.44 in magnitude (). A previous observation by Argentine astronomer Salvador Mazzone at the Observatorio Astronómico Salvador gave a similar period of with an amplitude of 0.42 in magnitude ().
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A rotational lightcurve of Severny was obtained by French amateur astronomer Laurent Bernasconi in March 2005. It gave a rotation period of 14.11 hours with a brightness variation of 0.14 magnitude (). In September 2013, photometric observations in the R-band at the Palomar Transient Factory, California, gave a shorter period of 9.2481 hours with an amplitude of 0.17 magnitude ().
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In January 1984, the first and best-rated rotational lightcurve of Sniadeckia was obtained from photometric observations by astronomer Richard Binzel. Lightcurve analysis gave a rotation period of 17.57 hours with a brightness variation of 0.16 magnitude (). French amateur astronomer Laurent Bernasconi measured an alternative period of 21.2 with an amplitude of 0.10 magnitude in April 2006 ().
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In April 2008, a rotational lightcurve of Wallonia was obtained from photometric observations by Brian Warner at the Palmer Divide Observatory in Colorado, United States. Lightcurve analysis gave a rotation period of hours with a brightness amplitude of 0.57 magnitude (). French amateur astronomer René Roy determined a very similar period of and an amplitude of 0.38 in April 2005 ().
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French amateur astronomer René Roy obtained a rotational lightcurve from photometric observations in October 2007. It gave a rotation period of hours with a brightness variation of 0.54 magnitude (), superseding observations by Brazilian Cláudia Angeli and by the Spanish ECLA project, which both gave a period of 7 hours with an amplitude of 0.57 and 0.4 magnitude, respectively ().
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WWVB transmits data at one bit per second, taking 60 seconds to send the current time of day and date within a century. There are two independent time codes used for this purpose: An amplitude-modulated time code, which has been in use with minor changes since 1962, and a phase- modulated time code added in late 2012.
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V428 Andromedae is the variable star designation for HD 3346. It is a short-period semi-regular variable (type SRS), also called an ultra- small-amplitude pulsating red giant. It has an amplitude of only 0.065 magnitudes. The main pulsation period is 11.5 days, but other periods of 11, 15, and 22 days have been detected.
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A rotational lightcurve of Peltier was obtained by Czech astronomer Petr Pravec at Ondřejov Observatory in October 2006. Lightcurve analysis gave a rotation period of 2.4287 hours with a brightness variation of 0.09 magnitude (). In December 2013, photometric observations by Australian amateur astronomer Julian Oey gave a concurring period of 2.4289 hours and an amplitude of 0.10 magnitude ().
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In May 2016, follow-up observation by Robert Stephens and Daniel Coley at the Center for Solar System Studies, California, and Linda French at Wesleyan University gave the so-far best rated period of hours with an amplitude of 0.47 (). Due to its higher than usual brightness variation, this Jovian asteroid is likely to have a non-spherical shape.
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Despite being usually referred to as a nova, it had characteristics that set it apart from other novae - an amplitude of at least 7 magnitudes, an unusually rapid decline in brightness and a location unusually far from the Galactic plane. Joseph Ashbrook suggested in 1953 that it may be a recurrent nova which has been observed only once.
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In August 2008, a rotational lightcurve of this asteroid was obtained by French amateur astronomer René Roy. Lightcurve analysis gave it a rotation period of 9.3209 hours with a change in brightness of 0.48 magnitude (). In November 2007, photometric observations at the U.S. Ricky Observatory (), Missouri, gave a refined period of 9.380 hours with an amplitude of 0.45 magnitude ().
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The switching scheme requires that both S+ and S- be on for a half cycle of the AC output period. The fundamental AC output amplitude is equal to '. Its harmonics have an amplitude of '. Therefore, the AC output voltage is not controlled by the inverter, but rather by the magnitude of the DC input voltage of the inverter.
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Several rotational lightcurve have been obtained since November 1990, when the first photometric observations of Paris – made by Italian astronomer Stefano Mottola, using the ESO 1-metre telescope at La Silla Observatory in Chile – gave a rotation period of hours with a brightness variation of magnitude. In July 1998, Mottola measured an identical period with an amplitude of 0.10 at Calar Alto Observatory in Spain (). Follow-up observations by Robert Stephens at the Center for Solar System Studies during 2016–2017 measured a period of 7.048 and 7.091 hours, each with an amplitude of 0.11 magnitude (), superseding a period of 7.08 hours by René Roy and Federico Manzini reported in 2008 and 2009, respectively (). The low brightness variation measured in all photometric observations is also indicative of a spherical, rather than elongated shape.
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Lightcurve-based 3D-model of Amanda A rotational lightcurve of Amanda was obtained from photometric observations by European astronomers at the La Silla Observatory before 1995. Lightcurve analysis gave a well-defined rotation period of hours with a brightness variation of magnitude (). In October 2010, French amateur astronomer Maurice Audejean determined a concurring period of () hours with an amplitude of () magnitude (), while in August 2018, a further observation by the TESS-team reported a period of () hours and an amplitude of () magnitude (). In 2016, a modeled lightcurve gave a sidereal period of hours using data from the Uppsala Asteroid Photometric Catalogue, the Palomar Transient Factory survey, and individual observers, as well as sparse-in-time photometry from the NOFS, the Catalina Sky Survey, and the La Palma surveys .
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The orbital period of this asteroid is close to a 2:1 commensurability with Jupiter, which made it useful for perturbation measurements to derive the mass of the planet. Photometry measurements made at the Oakley Observatory during 2006 produced a lightcurve with a rotation period of and an amplitude of in magnitude. It has an estimated span of and a mass of .
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It is a semiregular variable with a brightness that varies over an amplitude of 0.m28 with periods of 30 and 275 days. After evolving away from the main sequence it has expanded to around 70 times the solar radius, and now shines with 1,515 times the luminosity of the Sun. The effective temperature of the outer atmosphere is 3,490 K.
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In August 2004, a rotational lightcurve of Jovita was obtained from photometric observations by . Lightcurve analysis gave a rotation period of hours with a brightness variation of magnitude, indicative of a rather spherical shape (). A lower rated period determination of hours with an amplitude of magnitude was made by French amateur astronomers René Roy and Laurent Bernasconi in September 2004 ().
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In August 2012, a rotational lightcurve of Ilsewa was obtained from photometric observations by Robert Stephens at the Santana Observatory . Additional observations were taken at the Center for Solar System Studies . Lightcurve analysis gave a rotation period of hours with a brightness variation of magnitude (). Andrea Ferrero at Bigmuskie Observatory determined a concurring period of hours and an amplitude of magnitude.
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Observation of the asteroid light curve indicates it is rotating with a period of . During this interval, the magnitude varies by an amplitude of 0.12 ± 0.02. By combining the results of multiple light curves, the approximate ellipsoidal shape of the object can be estimated. It appears to be slightly elongated, being about 28.2% longer along one axis compared to the other two.
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Published in 1991, a first rotational lightcurve of Coppernicus was obtained by Polish astronomer Wiesław Wiśniewski. Lightcurve analysis gave a relatively short rotation period of 3.967 hours with a brightness variation of 0.22 magnitude (). In 2006, photometric observations by Italian astronomer Federico Manzini gave a tentative period of 5.37 and 5.375 hours with an amplitude of 0.01 and 0.04, respectively ().
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In November 2011, a rotational lightcurve of Hanoi was obtained from photometric observations made American astronomer by Brian Warner at his Palmer Divide Observatory in Colorado. The lightcurve gave a rotation period of hours with a brightness variation of 0.72 magnitude (). Ten years later, remeasurements of the original images rendered a slightly refined period of and an amplitude of 0.77 ().
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In August 2000, a rotational lightcurve of Imperatrix was obtained from photometric observations at the River Oaks Observatory () in Texas. Lightcurve analysis gave a rotation period of 13.34 hours with a brightness variation of 0.23 magnitude (). In September 2011, photometric observations by French amateur astronomers Pierre Antonini and René Roy gave a refined period of 17.769 hours with an amplitude of 0.21 magnitude ().
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Photometric observations made by American astronomer Robert Stephens in June 2003 at the Santana Observatory () in Rancho Cucamonga, California, gave a synodic rotation period of 13.83 hours and a brightness variation of 0.33 magnitude (). In May 2014, a lightcurve obtained by Brian Warner at the Palmer Divide Station () gave a divergent period of 5.633 hours with an amplitude of 0.13 ().
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In September 2012, a rotational lightcurve of Buie was obtained from photometric observations made at the Palomar Transient Factory, California. In the R-band, it gave a rotation period of hours with a brightness variation of 0.51 magnitude, while in the SG-Band the period was hours with an amplitude of 0.53 magnitude (). A high brightness variation typically indicates a non- spherical shape.
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In May 2016, a rotational lightcurve of Androgeos was obtained from photometric observations by Robert Stephens at the Center for Solar System Studies in California. Lightcurve analysis gave a rotation period of hours with a brightness amplitude of 0.37 magnitude (). This result supersedes similar period determinations with an amplitude of 0.31 and 0.64 by Stefano Mottola (1992) Stephens (2015), respectively ().
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In December 2009, and May 2012, two rotational lightcurves of Akhmatova were obtained from photometric observations by Czech astronomer Petr Pravec. Lightcurve analysis showed a rotation period of and hours with a brightness variation of 0.30 and 0.24 in magnitude, respectively (). Observations at the Palomar Transient Factory in August 2012, gave a period of hours and an amplitude of 0.40 in magnitude ().
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Astronomers Pierre Antonini and Silvano Casulli obtained a rotational light-curve of Beyer from photometric observations taken in July 2009. It gave a rotation period of 13.29 hours with a brightness variation of 0.35 magnitude (). In October 2010, observations in the R-band at the Palomar Transient Factory gave a similar period of 13.2608 hours and an amplitude of 0.12 magnitude ().
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In November 2005, a rotational lightcurve of Chaika was obtained from photometric observations by Italian astronomers Roberto Crippa, Federico Manzini and Josep Coloma. Lightcurve analysis gave a rotation period of hours with a brightness variation of 0.18 magnitude (). John Menke in collaboration with Walter Cooney and David Higgins determined a concurring period of hours with an amplitude of 0.20 magnitude ().
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In November 2006, a rotational lightcurve of Mayrhofer was obtained from observations taken by French amateur astronomer Pierre Antonini, giving a rotation period of 22.194 hours with a brightness variation of 0.45 in magnitude (). Photometric observation in the R-band at the Palomar Transient Factory in November 2011, gave a shorter period of 19.0808 hours with an amplitude of 0.30 magnitude ().
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In October 2010, a rotational lightcurve of Raywilson was obtained in the R-band from photometric observations by astronomers at the Palomar Transient Factory in California. Lightcurve analysis gave a rotation period of 4.654 hours with a brightness variation of 0.30 magnitude (). A previous measurement by Brazilian astronomers gave a period of 4.86 hours and an amplitude of 0.31 magnitude ().
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In November 2008, a rotational lightcurve of Kasan was obtained from photometric observations by American astronomer Robert Stephens. Lightcurve analysis gave a well-defined rotation period of 5.82 hours with a brightness variation of 0.25 magnitude (). Previously, a period of 5.83 hours with an amplitude of 0.26 magnitude was measured by Brian Warner at the Palmer Divide Observatory in September 2004 ().
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In February 2007, a rotational lightcurve of Kevola was obtained from photometric observations by French amateur astronomer Pierre Antonini. Lightcurve analysis gave a rotation period of 20.082 hours with a brightness variation of 0.23 magnitude (). Another lightcurve obtained by astronomers at the Palomar Transient Factory in October 2010, gave a concurring period of 20.071 hours with an amplitude of 0.33 magnitude ().
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Klimesh is a slow rotator, as it has a rotation period of 101 hours with a brightness variation of magnitude. The photometric observations were made by Czech astronomer Petr Pravec at the Ondřejov Observatory during the asteroid's 2011-opposition (). The result supersedes a period of 4.4 hours with an amplitude of 0.12, obtained from a fragmentary lightcurve by Italian astronomer Silvano Casulli ().
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In September 2010, a photometric lightcurve analysis of Modra by American astronomer Brian Warner at his Palmer Divide Observatory, Colorado, rendered an unambiguous period of hours with a brightness variation of 0.53 in magnitude (). A second lightcurve obtained during the wide-field survey at the U.S. Palomar Transient Factory in August 2010, and gave a period of hours with an amplitude of 0.42 ().
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In March 2004, a first rotational lightcurve of Amaryllis was obtained from photometric observations by French amateur astronomer René Roy. Lightcurve analysis gave a rotation period of 18.2 hours with a brightness variation of 0.20 magnitude (). In May 2016, the Spanish amateur astronomer group OBAS (Asteroid Observers, ) measured a refined period of 18.111 hours with an amplitude of 0.19 magnitude ().
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In 2001, a first, fragmentary lightcurve of Brita was published by a group of Brazilian and Argentine astronomers. Lightcurve analysis gave a rotation period of 5.8 hours with a brightness variation of 0.38 magnitude (). Between 2008 and 2016, photometric observations gave three well-defined periods of 5.805, 5.8158 and 5.8169 hours and an amplitude of 0.19, 0.23 and 0.20 magnitude, respectively ().
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In October 2007, a rotational lightcurve of Beljawskya was obtained by French amateur astronomer Pierre Antonini. It gave a well-defined rotation period of 6.284 hours with a brightness variation of 0.37 magnitude (). Photometric observations in the R-band at the U.S. Palomar Transient Factory in September 2013, gave a concurring period of 6.285 hours with an amplitude of 0.32 magnitude ().
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In March 2005, a rotational lightcurve of Róka was obtained from photometric observations by French amateur astronomer René Roy. Lightcurve analysis gave a rotation period of 10.04 hours with a brightness variation of 0.34 magnitude (). One month later, astronomer at the Rose-Hulman Observatory obtained another lightcurve with a concurring period of 10.09 hours and an amplitude of 0.40 magnitude ().
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In December 2010, a rotational lightcurve was obtained for this asteroid from photometric observations at the U.S. Palomar Transient Factory, California. It gave a rotation period of hours with a brightness variation of 0.35 magnitude (). A second lightcurve, obtained by Italian amateur astronomer Silvano Casulli in August 2014, gave a concurring period of hours with an amplitude of 0.38 in magnitude ().
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In March 2011, a rotational lightcurve of Neujmina was obtained from photometric observations at the Oakley Southern Sky Observatory in Australia. Lightcurve analysis gave a well-defined rotation period of 5.0844 hours with a brightness variation of 0.20 magnitude (). Previous measurements in 1984 and 2008, gave a period of 5.089 and 7.61 hours with an amplitude of 0.15 and 0.06 magnitude, respectively ().
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In September 2007, photometric observations at the Oakley Observatory in Indiana, United States, gave a fragmentary lightcurve with a rotation period of 10.07 hours and a brightness variation of 0.15 magnitude (). Another fragmentary lightcurve of Simona was obtained by French amateur astronomer René Roy in August 2012. Lightcurve analysis gave a period of 9.6 hours with an amplitude of 0.02 magnitude ().
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A rotational lightcurve of Bobweber was obtained from photometric observations by Czech astronomer Petr Pravec at Ondřejov Observatory in December 2009. It gave a well-defined rotation period of hours with a brightness variation of 0.12 in magnitude (). In January 2014, astronomer Julian Oey at the Australian Blue Mountains Observatory () obtained a nearly identical period of hours with an amplitude of 0.15 magnitude ().
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Neptune's small moon Galatea, which orbits just inside of the Adams ring at 61,953 km, acts like a shepherd, keeping ring particles inside a narrow range of orbital radii through a 42:43 outer Lindblad resonance. Galatea's gravitational influence creates 42 radial wiggles in the Adams ring with an amplitude of about 30 km, which have been used to infer Galatea's mass.
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In September 2003, a rotational lightcurve of Scythia was obtained from photometric observations by Robert Stephens at the Santana Observatory in California. Lightcurve analysis gave a rotation period of 15.05 hours with a brightness variation of 0.15 magnitude (). In August 2008, Pierre Antonini measured a better period solution of 7.525 hours (or half the period) and an amplitude of 0.25 magnitude ().
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In October 1989, the first photometric observations of Saunders were made with the ESO 1-metre telescope at La Silla in Chile. It gave a rotation period of 6 hours with a brightness variation of 0.3 magnitude (). Another rotational lightcurve was obtained by Czech astronomer Petr Pravec at Ondřejov Observatory in August 2003, giving a period of and an amplitude of 0.2 magnitude ().
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Geographic features on the Aleppo plateau The average elevation of the plateau is 400 m. The surface gradually slopes down in north-south and west-east directions. The surface undulates gently with an amplitude of 10-30 m for each wave. The lowlands are covered with combined Paleozoic and Mesozoic sediments that average 4-5 km in thickness over the whole surface.
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In July 2007, astronomer Lorenzo Franco obtained a rotational lightcurve of Wilkens at the Balzaretto Observatory () near Rome, Italy. It gave a well-defined period of 7.248 hours and a brightness variation of 0.23 magnitude (). Photometric observations in the S-band at the Palomar Transient Factory in January 2014, gave a period of 7.3017 hours with an amplitude of 0.34 ().
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In April 2014, a rotational lightcurve of Yeomans was obtained from photometric observations made at the Isaac Aznar Observatory in Spain. Lightcurve analysis gave a rotation period of 3.4 hours with a brightness variation of 0.28 magnitude (). A similar period of 3.509 hours with an amplitude of 0.24 magnitude was found by astronomers at the Palomar Transient Factory in October 2011 ().
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In May 2006, a rotational lightcurve of Weir was obtained from photometric observations by Brian Warner at his Palmer Divide Observatory in Colorado. Lightcurve analysis gave a rotation period of 14.602 hours with a brightness variation of 0.18 magnitude (). A concurring period of 14.657 hours and an amplitude of 0.24 magnitude was measured by astronomers at the Palomar Transient Factory in May 2010 ().
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In March 2014, a rotational lightcurve was obtained from photometric observations at the U.S. Burleith Observatory in Washington D.C.. It gave a well-defined rotation period of 11.1 hours with a brightness variation of 0.25 magnitude () A previous fragmentary lightcurve obtained by French amateur astronomer Laurent Bernasconi in May 2006, gave a much shorter period of 6.6 hours with an amplitude of 0.06 ().
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In July 2006, a rotational lightcurve of Swann was obtained from photometric observations by Petr Pravec at the Ondřejov Observatory in the Czech Republic. It gave a rotation period of hours with a brightness variation of 0.67 magnitude (). A second lightcurve obtained by Jean-Gabriel Bosch in September 2006, gave a period of hours and an amplitude of 0.35 magnitude ().
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In September 2001, a rotational lightcurve of Tselina was obtained from photometric observations by French amateur astronomer Laurent Bernasconi. Lightcurve analysis gave a well-defined rotation period of hours with a brightness variation of 0.17 magnitude (). In September 2012, observations by astronomers at the Palomar Transient Factory, California, gave a concurring period of hours with an amplitude of 0.29 magnitude ().
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The first rotational light curve of Kutaïssi was obtained from photometric observations by American astronomer Richard Binzel in February 1984. It gave a rotation period of 3.60 hours with a brightness variation of 0.40 magnitude (). In 1987 and 2004, a group of American astronomers obtained concurring light curves with a period of and hours and an amplitude of 0.30 and 0.42 magnitude, respectively ().
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French amateur astronomer Laurent Bernasconi obtained a lightcurve of Beograd from photometric observations taken in March 2005. Light-curve analysis gave a rotation period of 6.943 hours with a brightness variation of 0.18 magnitude (). In April 2014, a lightcurve obtained by Vladimir Benishek at the discovering Belgrade Observatory gave a concurring period of 6.9490 hours with an amplitude of 0.23 magnitude ().
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By describing the spin-chain as an amplitude damping channel, it is possible to calculate the various capacities associated with the channel. One useful property of this channel, which is used to find these capacities, is the fact that two amplitude damping channels with efficiencies \eta and \eta' can be concatenated. Such a concatenation gives a new channel of efficiency \eta\eta'.
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Photometric observations of this asteroid by Slovak astronomer Adrián Galád in September 2006, gave a rotational lightcurve with a rotation period of hours and a brightness variation of magnitude (). A second, less secure lightcurve was obtained by Italian astronomers Roberto Crippa and Federico Manzini in September 2013, which gave a divergent period of hours with an amplitude of 0.46 magnitude ().
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In December 2014, astronomer Maurice Clark obtained a rotational lightcurve from photometric observations at Preston Gott Observatory. Lightcurve analysis gave an ambiguous rotation period of 18.3980 hours with a brightness variation of 0.41 magnitude, suggesting a non-spheroidal shape (). The alternative period solution is 9.14 hours with an amplitude of 0.32 magnitude. The results supersede a previously obtained period of 5.547 hours ().
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Recent calculations indicate that it is a stable Mars trojan with a libration period of 1300 yr and an amplitude of 18°. These values as well as its short-term orbital evolution are similar to those of 5261 Eureka. Its eccentricity oscillates mainly due to secular resonances with the Earth and the oscillation in inclination is likely driven by secular resonances with Jupiter.
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Three rotational lightcurves of Tynka were independently obtained from photometric observations by astronomers David Higgins, Agnieszka Kryszczyńska and Robert Stephens. Lightcurve analysis gave a rotation period of 11.75 and 11.893 hours with a brightness variation between 0.06 and 0.33 magnitude (). An alternative period solution of 5.9818 hours with an amplitude of 0.17 was measured by French amateur astronomer René Roy in April 2012 ().
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9 Cephei (9 Cep), also known as V337 Cephei, is a variable star in the constellation Cepheus. 9 Cephei was given the name V337 Cephei and classified as an α Cygni variable in 1967. It varies irregularly between magnitude 4.69 and 4.78. A study of the Hipparcos satellite photometry showed an amplitude of 0.56 magnitudes, but could find no periodicity.
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In September 2007, a rotational lightcurve of Figneria was obtained by astronomer Julian Oey at the Kingsgrove () and Leura Observatories () in Australia. Lightcurve analysis gave a rotation period of 13.577 hours with a brightness variation of 0.16 magnitude (). In January 2014, photometric observations at the Palomar Transient Factory in California gave a period of 13.583 hours and an amplitude of 0.15 magnitude ().
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In telecommunication, the term white facsimile transmission has the following meanings: # In an amplitude-modulated facsimile system, transmission in which the maximum transmitted power corresponds to the minimum density, i.e., the white area, of the object. # In a frequency-modulated facsimile system, transmission in which the lowest transmitted frequency corresponds to the minimum density i.e., the white area, of the object.
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In time, it became possible to construct radar maps from topographic maps. Preparation of the maps required the route to be flown by an aircraft. A radar on the aircraft was set to a fixed angle and made horizontal scans of the land in front. The timing of the return signal indicated the range to the landform and produced an amplitude modulated (AM) signal.
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In April 2013, a rotational lightcurve of ' was obtained from photometric observations by Robert Stephens at the Center for Solar System Studies (CS3) in California. Lightcurve analysis gave a rotation period of hours and a brightness variation of 0.30 magnitude (). Observations by his college Brian Warner at CS3 in July 2017, gave a similar period of 12.530 hours with an amplitude of 0.25 magnitude ().
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In September 2006, a rotational lightcurve of Naëma was obtained from photometric observations by Collin Bembrick at the Mount Tarana Observatory , Australia, in collaboration with Bill Allen and Greg Bolt. Lightcurve analysis gave a relatively long rotation period of hours with a brightness variation of magnitude (). In December 2017, French amateur astronomer René Roy determined a lower-rated, tentative period of hours with an amplitude of magnitude ().
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In April 2008, a rotational lightcurve of Leopoldina was obtained from photometric observations by Brian Warner at the Palmer Divide Observatory in Colorado. Analysis gave a classically shaped bimodal lightcurve with a well-defined rotation period of hours and a brightness variation of magnitude (). The result supersedes Warner's previous observation from August 2005, which determined a period of hours and an amplitude of magnitude ().
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In June 2018, a rotational lightcurve of Sphinx was obtained from photometric observations by Tom Polakis at the Command Module Observatory in Arizona. Lightcurve analysis gave a rotation period of hours with a brightness variation of magnitude (). However, an alternative period solution of hours with an amplitude of magnitude is also possible. Both results supersede a tentative period determination by Laurent Bernasconi from September 2001 ().
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Nu¹ Sagittarii A is a spectral type K1 bright giant which has an apparent magnitude of +4.86. It is a microvariable with a frequency of 0.43398 cycles per day and an amplitude of 0.0078 magnitude. In 1982 it was found to have a hotter companion, Nu¹ Sagittarii B, a rapidly rotating B9 type star. The pair orbit with a period of around 370 days.
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An analysis of Hipparcos photometry showed an amplitude of 0.0168 magnitudes and a period of 2.65 days. The statistical signal was strong enough for the variability to be very likely, but 5 Persei has not formally been catalogued as a variable star. 5 Persei has two nearby companions, a 12th magnitude star 5.7 arc-seconds away and a 13th magnitude star one arc-minute away.
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In February 2007, a rotational lightcurve of Birgit was obtained from photometric observations by Agnieszka Kryszczyńska at Poznań Observatory, Poland, and international collaborators. Lightcurve analysis gave a rotation period of hours with a brightness variation of magnitude (). The result supersedes observations by Federico Manzini, Roberto Crippa, and Pierre Antonini from August 2005, who determined a poorly rated period of hours with an amplitude of magnitude ().
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In December 2005, a rotational lightcurve of Romilda was obtained from photometric observations over seven nights by Walter Cooney at the Blackberry Observatory in Louisiana. Lightcurve analysis gave a rotation period of hours with a brightness variation of magnitude (). In January 2006, Italian astronomers Roberto Crippa and Federico Manzini at the Sozzago Astronomical Station determined a nearly identical period of hours with an amplitude of magnitude ().
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Delta Scuti (δ Sct) variables are similar to Cepheids but much fainter and with much shorter periods. They were once known as Dwarf Cepheids. They often show many superimposed periods, which combine to form an extremely complex light curve. The typical δ Scuti star has an amplitude of 0.003–0.9 magnitudes (0.3% to about 130% change in luminosity) and a period of 0.01–0.2 days.
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Beta Cephei (β Cep) variables (sometimes called Beta Canis Majoris variables, especially in Europe)Variable Star Of The Season, Winter 2005: The Beta Cephei Stars and Their Relatives, John Percy, AAVSO. Accessed October 2, 2008. undergo short period pulsations in the order of 0.1–0.6 days with an amplitude of 0.01–0.3 magnitudes (1% to 30% change in luminosity). They are at their brightest during minimum contraction.
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It has a rotation period of and a lightcurve with an amplitude of 0.18 mag. The lightcurve shows 4 maxima and 4 minima per cycle, suggesting an irregular shape. The previously accepted period of 10.42 hours with 2 maxima and minima per cycle was proven to be wrong by Pilcher in 2016, showing that correct rotation periods still have not been found for all low-numbered asteroids.
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Several rotational lightcurves of Kanaya have been obtained from photometric observations. In December 2005, a first lightcurve by astronomer David Higgins at Hunters Hill Observatory (), Australia, gave a rotation period of hours with a brightness variation of 0.22 magnitude (). In October 2010, Czech astronomer Petr Pravec obtained another well-defined period of hours with an amplitude of 0.16 magnitude (). Other observations rendered similar periods ().
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In 1977, a rotational lightcurve of Geertruida was obtained from photometric observations by Swedish astronomer Claes-Ingvar Lagerkvist at the Uppsala Southern Station in Australia. Lightcurve analysis gave a rotation period of 5.50 hours with a brightness amplitude of 0.5 magnitude (). In October 2016, a refined period of 5.5087 hours with an amplitude of 0.35 magnitude () was obtained at the Oakley Southern Sky Observatory ().
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In January 2008, a rotational lightcurve of Geowilliams was obtained from photometric observations by Australian amateur astronomer David Higgins at the Hunters Hill Observatory . Lightcurve analysis gave a well-defined rotation period of 14.387 hours with a brightness variation of 0.40 magnitude (). In July 2010, a similar period of 14.383 hours and an amplitude of 0.42 was measured at the Palomar Transient Factory in California ().
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Photometric observations of Ilioneus were obtained by Stefano Mottola in February 1994. Lightcurve analysis gave a rotation period of hours with a brightness amplitude of 0.16 magnitude (). Follow-up observations by astronomers at the Palomar Transient Factory in 2013, and by Robert D. Stephens at the Center for Solar System Studies in 2015 and 2017, gave a concurring period determination with an amplitude between 0.18 and 0.34 ().
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The moon's diameter was estimated to be 21% of that of Huntress (or 1.3 kilometers assuming a primary diameter of 6 km). In March 2012, Australian astronomer David Higgins obtained a concurring lightcurve with period of 2.44 hours and an amplitude of 0.11 magnitude (). For an asteroid of its size, Huntress has a relatively short spin rate, not much above the 2.2-hour threshold for fast rotators.
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In September 2008, a rotational lightcurve of Amanogawa was obtained from photometric observations at the Oakley Southern Sky Observatory and Oakley Observatory. Lightcurve analysis gave a well- defined rotation period of 12.38 hours with a brightness variation of 0.48 magnitude (). In February 2014, astronomers at the Palomar Transient Factory measured a similar period of 12.369 hours and an amplitude of 0.38 magnitude in the R-band ().
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A rotational lightcurve of Akka was obtained from photoelectric observation made by Polish astronomer Wiesław Wiśniewski of the University of Arizona in August 1992. The ambiguous lightcurve gave a rotation period of hours with a brightness variation of 0.46 in magnitude (). Alternatively, the body rotates once every hours (or half the previous period) with an amplitude of 0.52, as determined by Czech astronomer Petr Pravec ().
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From 2005 to 2015, several astronomers such as Donald Pray, Henk de Groot and Raoul Behrend, Federico Manzini, as well as Laurent Bernasconi unsuccessfully tried to obtain a well-defined lightcurve of Alfaterna. While Pray derived a period of 3.664 hours with an amplitude of 0.05 magnitude (), the European astronomers published a tentative period of 33.12 hours (). As of 2017, the body's spin rate effectively remains unknown.
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In December 2014, a rotational lightcurve of Alvema was obtained from photometric observations by French amateur astronomer Laurent Bernasconi. It gave a rotation period of with a brightness variation of 0.33 magnitude (). The asteroid's first lightcurve was reported by astronomer Darryl Sergison at the Gothers Observatory () in the United Kingdom, from observations made in November 2009, showing a period of hours with an amplitude of 0.17 magnitude ().
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In February 2010, a rotational lightcurve of Ceragioli was obtained from photometric observations in the R-band by astronomers at the Palomar Transient Factory in California. Lightcurve analysis gave a rotation period of hours with a brightness variation of 0.35 magnitude (), indicative of an elongated shape. Also in February 2010, David Polishook determined a similar period of hours with an amplitude of 0.25 magnitude ().
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In August 1984, a first rotational lightcurve of Pierre was obtained from photometric observations with the ESO 1-metre telescope at the La Silla Observatory in Chile. Lightcurve analysis gave a rotation period of 18 hours with a brightness variation of 0.09 magnitude (). A poorly rated lightcurve by Pierre Antonini in Januar 2007, gave a period of 24 hours with an amplitude of 0.05 magnitude.
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In April 2001, astronomer Colin Bembrick obtained the first rotational lightcurve of Pannonia at Tarana Observatory in Australia. Lightcurve analysis gave a well-defined rotation period of 10.756 hours with a brightness amplitude of 0.16 magnitude (). In 2002 and 2004, photometric observations by French astronomers Laurent Bernasconi and Bernard Christophe Additional periods of 6.2 and 6.205 hours with an amplitude of 0.57 and 0.37, respectively ().
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Klare has been the subject of multiple photometric lightcurve studies, which gave a well-determined rotation period between 4.741 and 4.744 hours with a brightness variation between 0.70 and 0.90 magnitude (). Measurements have also been used as the basis for generating a three- dimensional model of its shape. The Collaborative Asteroid Lightcurve Link (CALL) adopts a period 4.744 hours with an amplitude of 0.70 magnitude ().
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In September 2002, a first rotational lightcurve of Malmquista was obtained from photometric observations by Stephen Brincat at Flarestar Observatory on the island of Malta. Lightcurve analysis gave a well-defined rotation period of 14.077 hours with a brightness variation of 0.60 magnitude (). In September 2012, observations at the Palomar Transient Factory, California, gave a period of 14.044 hours and an amplitude of 0.42 magnitude ().
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In the 1990s, a rotational lightcurve of Marina was obtained from a survey of Hildian asteroids by European astronomers. Lightcurve analysis gave a well-defined rotation period of 9.45 hours with a brightness variation of 0.29 magnitude (). In October 2010, photometric observations in the R-band by astronomers at the Palomar Transient Factory in California gave a similar period of 9.571 hours and an amplitude of 0.09 ().
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A rotational lightcurve of Niels was obtained by astronomer Maurice Clark in December 2005. It gave it a rotation period of 9.976 hours with a brightness variation of 0.15 magnitude (). In November 2008, photometric observations by amateur astronomer Pierre Antonini gave another period of 19.2 hours with an amplitude of 0.01 (). As of 2017, a secure period for Niels has not yet been obtained.
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In March and April 2007, two rotational lightcurves of Nurmela was obtained from photometric observations by Adrián Galád and Robert Stephens. They gave an identical rotation period of 3.1587 hours with a brightness variation of 0.33 and 0.42 magnitude, respectively (). In April 2017, another observation by Stephens gave a concurring period of 3.159 hours () with an amplitude of 0.58 magnitude, indicative for an elongated shape.
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In September 2008, a rotational lightcurve of Milton was obtained from photometric observations by Julian Oey at the Kingsgrove and Leura observatories. Lightcurve analysis gave a rotation period of 3.2978 hours with a brightness variation of 0.30 magnitude (). In August 2012, a refined period of 3.295 hours and an amplitude of 0.16 magnitude was measured by Afşar Kabaş at the Çanakkale University Observatory in Turkey ().
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In May 2017, a rotational lightcurve of Tunica was obtained from photometric observations by French amateur astronomer René Roy. Lightcurve analysis gave a rotation period of 15.8 hours with a brightness variation of 0.24 magnitude (). Another lightcurve obtained in the R-band by astronomers at the Palomar Transient Factory in February 2010 gave a period of 15.673 hours and an amplitude of 0.32 magnitude ().
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Observations performed by Brian Warner at the Palmer Divide Observatory in Colorado Springs, Colorado, during 2007 produced a lightcurve with a period of 10.080 ± 0.005 hours and a brightness range of 0.17 ± 0.02 in magnitude (). Another lightcurve obtained by Italian amateur astronomers Roberto Crippa and Federico Manzini at the Sozzago Astronomical Station () gave a period of 9.0127 hours with an amplitude of 0.17 magnitude ().
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In November 2004, a rotational lightcurve of Aethusa was obtained from photometric observations by French amateur astronomer René Roy at Blauvac Observatory (). Lightcurve analysis gave a rotation period of 12.916 hours with a brightness variation of 0.12 magnitude (), while in March 2006, astronomer Brian Warner at his Palmer Divide observatory in Colorado, United States, obtained a shorter period of 8.621 hours and an amplitude of 0.18 magnitude ().
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9 Equulei is an M-type star in the constellation Equuleus. It is an asymptotic giant branch (AGB) star, a star that has exhausted its core helium and is now fusing both hydrogen and helium in shells outside the core. It is also a suspected variable star with an amplitude of about 0.05 magnitudes. The spectral type is M2IIIa, meaning it is a relatively cool giant star.
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Photometric measurements of Marlene – made by American astronomer Brian Warner at the Palmer Divide Observatory (), Colorado, in February 2005 – showed a lightcurve with a longer-than average rotation period of hours and a brightness variation of in magnitude (). Most asteroids have periods shorter than 20 hours. Another lightcurve, obtained by French amateur astronomer René Roy, gave a period of 29.0 hours and an amplitude of 0.17 magnitude ().
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In August 2012, a rotational lightcurve of Barks was obtained from photometric observations by astronomers at the Oakley Southern Sky Observatory () in Australia. Lightcurve analysis gave a well- defined rotation period of 6.084 hours with a brightness variation of 0.26 magnitude (). This concurs with observations taken at the Palomar Transient Factory in January 2011, which gave a period of 6.087 hours and an amplitude of 0.28 magnitude ().
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The radius determined from the observed brightness and colour of the star is . 15 Arietis is a short period semiregular variable with the designation AV Arietis. The period given in the General Catalogue of Variable Stars is 5.032 days. Longterm photometry finds that the strongest pulsation period is 18.1 days with an amplitude of 0.028 magnitudes, while a second is 21.9 days and 0.030 in magnitude.
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In October 2010, a rotational lightcurve of Arago was obtained from photometric observations that was later submitted to the CALL website. Lightcurve analysis gave a rotation period of 8.7819 hours with a brightness amplitude of 0.22 magnitude (). In April 2016, another lightcurve was obtained by the group of Spanish amateur astronomers OBAS. It gave a concurring period of 8.784 hours with an amplitude of 0.22 magnitude ().
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In May 1984, a first rotational lightcurve of Irmela was obtained from photometric observations by American astronomer Richard Binzel. Lightcurve analysis gave a rotation period of 19.17 hours with a brightness variation of 0.34 magnitude (). In March 2010, astronomer Robert Stephens obtained another lightcurve at the Center for Solar System Studies, that gave a divergent period of 11.989 hours with an amplitude of 0.40 magnitude ().
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In February 2004, a rotational lightcurve of Aquilegia was obtained from photometric observations by French amateur astronomer Laurent Bernasconi. Lightcurve analysis gave a well-defined rotation period of 5.792 hours with a high brightness variation of 0.75 magnitude (), indicative for a non-spherical shape. Previous observations by Richard Binzel in May 1984 gave a similar period of 5.79 hours and an amplitude of 0.93 magnitude ().
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In May 2009, a rotational lightcurve of Voloshina was obtained from photometric observations by astronomers at the Oakley Southern Sky Observatory () in Australia. Lightcurve analysis gave a rotation period of 5.896 hours with a brightness variation of 0.40 magnitude (). In January and February 2014, astronomers at the Palomar Transient Factory found a period of and hours with an amplitude of 0.32 and 0.27 magnitude, respectively ().
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This is an evolved red giant star with a stellar classification of M4.5 IIIa. It is a pulsating variable with multiple periods, including 20.6, 24.1, 24.5, and 32.3 days. The strongest period is 33.3 days with an amplitude of 0.043 magnitude. It has a magnitude 9.71 visual companion at an angular separation of 60.4 arc seconds along a position angle of 210°, as of 2013.
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In October 2005, a rotational lightcurve of Akasofu was obtained from photometric observations made by David Higgins at Hunters Hill Observatory, Australia. It showed a rotation period of hours with a brightness variation of 0.10 in magnitude (). Observations by Czech astronomer Petr Pravec in March 2007, gave another well-defined and concurring lightcurve with a period of hours and an amplitude of 0.15 in magnitude ().
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Two rotational lightcurves of Aditi were obtained from photometric observations by American astronomer Brian Warner at his Palmer Divide Observatory, Colorado, in August 2014 and March 2015, respectively. The first lightcurve rendered a period of hours with a brightness variation of 0.64 (), while the second one gave a period of hours with an amplitude of 0.29 magnitude (). Additional lightcurves were obtained by Benishek () and Manzini ().
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In September 1983, a first rotational lightcurve of Saimaa was obtained from photometric observations by American astronomer Richard Binzel at CTIO and McDonald Observatory. Lightcurve analysis gave a well-defined rotation period of 7.08 hours with a brightness variation of 0.18 magnitude (). In February 2007, another lightcurve obtained by French amateur astronomer René Roy gave a concurring period of 7.1181 hours and an amplitude of 0.26 magnitude ().
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In December 2010, a rotational lightcurve of Shanghai was obtained for this asteroid from photometric observations taken at the U.S. Palomar Transient Factory in California. It gave a rotation period of hours with a brightness variation of 0.16 magnitude (). One month later in January 2011, a similar period of hours with an amplitude of 0.16 magnitude was derived by French amateur astronomer Pierre Antonini ().
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In July 2013, a rotational lightcurve of Shao was obtained from photometric observations by Italian amateur astronomer Silvano Casulli. Lightcurve analysis gave a rotation period of 7.452 hours with a brightness variation of 0.15 magnitude (). A second lightcurve by astronomers at the Palomar Transient Factory from December 2014, gave a shorter period of 5.61 hours and an amplitude of 0.11 (), indicative for a rather spherical shape.
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In 2010 and 2013, two rotational lightcurves of Shkodrov have been obtained by astronomers at the Palomar Transient Factory in California. Lightcurve analysis of the photometric observations in the R-band gave a rotation period of 17.256 and 17.302 hours with a brightness variation of 0.40 and 0.35 magnitude, respectively (). In 2015, Petr Pravec published a refined period of 17.3233 hours and an amplitude of 0.42 magnitude ().
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In March 2009, a rotational lightcurve of Stobbe was obtained from photometric observations made by French amateur astronomer Pierre Antonini at his Observatoire de Bédoin rendered a well-defined period of hours with a brightness variation of 0.35 in magnitude (), superseding a previous observation at the Roach Motel Observatory () in Riverside, California, that gave a period of hours and an amplitude of 0.27 in magnitude ().
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Tina has a well-defined rotation period of 13.395 hours with a brightness variation of 0.18 magnitude (), derived from photometric observations taken by American astronomer Brian Warner at his Palmer Divide Observatory, Colorado, in September 2007 (also see ). Other lightcurves were obtained by French amateur astronomers Pierre Antonini and Jean-Gabriel Bosch, which gave a period of 17.164 hours and an amplitude of 0.30 magnitude ().
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Observations performed by American astronomer Brian Warner at the Palmer Divide Observatory in Colorado Springs, Colorado, during February 2007 produced a lightcurve with a period of 19.50 ± 0.02 hours and an amplitude of 0.25 ± 0.02 in magnitude (). In September 2011, photometry in the S-band at the Palomar Transient Factory gave a similar period of 19.777 hours with a brightness variation of 0.18 magnitude ().
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Some signal processing techniques such as those used in radar may require both the amplitude and the phase of a signal, to recover all the information encoded in that signal. One technique is to feed an amplitude-limited signal into one port of a product detector and a reference signal into the other port; the output of the detector will represent the phase difference between the signals.
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The key to the Wien bridge oscillator's low distortion oscillation is an amplitude stabilization method that does not use clipping. The idea of using a lamp in a bridge configuration for amplitude stabilization was published by Meacham in 1938.. . Meacham presented his work at the Thirteenth Annual Convention of the Institute of Radio Engineers, New York City, June 16, 1938 and published in Proc. IRE October 1938.
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In the northern part, it decreases to 20–25‰ due to the inflow of fresh water from the Irrawaddy River. Tides are semidiurnal (i.e., rising twice a day) with an amplitude of up to 7.2 meters. Monthly averaged Ekman Pumping velocity (in m per day) for June and December The effect of wind stress on ocean surface is explained with the help of wind stress curl.
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In September 2001, the first ever conducted photometric observation of Bickel at the Rozhen Observatory, Bulgaria, rendered a rotational lightcurve with a longer-than-average period of hours and a brightness variation of 0.63 magnitude (). A more refined lightcurve was obtained in October 2005, by astronomers Raymond Poncy, Laurent Bernasconi and Rui Goncalves, which gave a well-defined period of hours with an amplitude of 0.72 magnitude ().
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In December 2009, a rotational lightcurve of Alconrad was obtained from photometric observations at the ground-based Wise Observatory in Mitzpe Ramon, Israel. Lightcurve analysis gave a rotation period of hours with a brightness variation of magnitude (). In October 2013, photometric observations by astronomers in the R-band at the Palomar Transient Factory in California gave a period of with an amplitude of magnitude ().
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A rotational lightcurve of Bobhope was obtained from photometric observations by astronomer Landy Carbo at Oakley Southern Sky Observatory , Australia, and at the U.S. Oakley Observatory in September 2008. It gave it a rotation period of hours with a brightness variation of magnitude (). A previously published lightcurve by French amateur astronomer Bernard Christophe gave a somewhat longer period of hours with an amplitude of 0.50 ().
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In January 2002, a rotational lightcurve of Andrée was obtained from photometric observations by French amateur astronomer Laurent Bernasconi. Lightcurve analysis gave a well-defined rotation period of 5.178 hours with a brightness variation of 0.27 magnitude (). In October 2004, a concurring lightcurve with a period of 5.18366 hours and an amplitude of 0.23 was obtained by French astronomers Cyril Cavadore and Pierre Antonini ().
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For analog radio, the switch to digital radio is made more difficult by the higher cost of digital receivers.DAB Products , World DAB Forum, 2006. The choice of modulation for analog radio is typically between amplitude (AM) or frequency modulation (FM). To achieve stereo playback, an amplitude modulated subcarrier is used for stereo FM, and quadrature amplitude modulation is used for stereo AM or C-QUAM.
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In September 2006, a rotational lightcurve for Palach was obtained from photometric observations made by French amateur astronomer Laurent Bernasconi at St. Michel sur Meu. It gave a rotation period of 3.139 hours with a brightness amplitude of 0.16 magnitude (). In May 2010, a second lightcurve, obtained by Zachary Pligge at Oakley Southern Sky Observatory, Australia, gave a period of 3.1358 hours with an amplitude of 0.13 ().
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A rotational lightcurve of Harrison was obtained from photometric observations by Czech astronomer Petr Pravec at Ondřejov Observatory in May 2015. It gave a well-defined rotation period of hours with a brightness variation of 0.42 in magnitude (). During the following month, photometric observations at three Italian observatories gave a second lightcurve with a period of hours and an amplitude of 0.37 in magnitude ().
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It has an absolute magnitude of −1.55. This is an evolved K-type giant star with a stellar classification of K5 III, which means it has used up its core hydrogen and has expanded. At present it has 40 times the radius of the Sun. It is a variable star of unknown type, with an amplitude of 0.008 in visual magnitude and a period of 4.82 days.
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Its changes in brightness are complex with at least two different periods showing. The General Catalogue of Variable Stars lists a period of 110 days. More recent studies show a primary pulsation period of 133 days, with and a long secondary period with an amplitude of 0.2 magnitudes and duration 1,300 days. The long secondary period variations are possibly caused by long-lived convection cells.
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In January 2010, a rotational lightcurve of ' was obtained from photometric observations by Pierre Antonini at the Bédoin Observatory in southeastern France. Lightcurve analysis gave a rotation period of hours with a brightness variation of 0.30 in magnitude (). A previous 2006-observation by American astronomer Brian Warner at his Palmer Divide Observatory in Colorado gave a period of hours and an amplitude of 0.24 magnitude ().
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Winds also induce frequent seiches – standing waves with an amplitude of 20–50 cm and lasting from minutes to hours. Another consequence of the winds is water currents. The prevailing current is a counterclockwise swirl due to the westerly and south-westerly winds. Their speed is typically less than 10 cm/s, but can reach 60–70 cm/s for 15–20 m/s winds.
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Several rotational lightcurves of Äneas have been obtained since the first photometric observations by William Hartmann in 1988, that gave a period of 8.33 hours, and by Stefano Mottola and Anders Erikson in 1993, using the ESO 1-metre telescope at La Silla Observatory in Chile. Lightcurve analysis gave a rotation period of hours with a brightness variation of magnitude (). In July and August 2008, Susan Lederer at CTIO in Chile, and Robert Stephens at the Goat Mountain Astronomical Research Station in California, determined a well-defined period of with an amplitude 0.20 magnitude (). Follow-up observations during 2015–2017 by Robert Stephens and Daniel Coley at the Center for Solar System Studies gave three concurring periods of 8.701, 8.681 and 8.7 hours with an amplitude of 0.62, 0.40 and 0.21 magnitude, respectively (), while in August 2011, Pierre Antonini reported a period of 11.8 hours based on a fragmentary lightcurve ().
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Erato (minor planet designation: 62 Erato) is a carbonaceous Themistian asteroid from the outer region of the asteroid belt, approximately in diameter. Photometric measurements during 2004–2005 showed a rotation period of with an amplitude of in magnitude. It is orbiting the Sun with a period of , a semimajor axis of , and eccentricity of 0.178. The orbital plane is inclined by an angle of 2.22° to the plane of the ecliptic.
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Panopaea (minor planet designation: 70 Panopaea) is a large main belt asteroid. Its orbit is close to those of the Eunomia asteroid family; however, Panopaea is a dark, primitive carbonaceous C-type asteroid in contrast to the S-type asteroids of the Eunomian asteroids. The spectra of the asteroid displays evidence of aqueous alteration. Photometric studies give a rotation period of 15.797 hours and an amplitude of in magnitude.
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It has a 2:1 commensurability with Mars, having an orbital period double that of the planet. The orbital plane lies at an inclination of 6.0° to the plane of the ecliptic. This is a stony S-type asteroid with a cross-sectional size of 61 km, Photometry from the Oakley Observatory during 2006 produced a lightcurve that indicated a sidereal rotation period of with an amplitude of in magnitude.
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801 Helwerthia is a C-type asteroid orbiting in the Main belt near the Eunomia family. However, it is not a family member but an un-related interloper in the region because its composition is inconsistent with membership. Its diameter is about 33 km, its albedo around 0.038. An international team of astronomers observed this minor planet photometrically in 2012, determining a rotation period of with an amplitude of in magnitude.
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Generally, the purpose of an interferometer is to transform a differential phase modulation (of two light beams) into an amplitude modulation of the output light . Accordingly, the injected vacuum-squeezed field is injected such that the differential phase quadrature uncertainty in the arms is squeezed. On the output light amplitude quadrature squeezing is observed. Fig. 4 shows the photo voltage of the photo diode in the interferometer output port.
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This is a blue supergiant of spectral type B5 Ia; a massive star that has used up its core hydrogen and expanded into a very luminous star. It has an effective temperature around 15,000 K and is radiating 83,000 times the Sun's luminosity. Several studies of 5 Persei have detected possible small amplitude variations. In 1983, an amplitude of 0.045 magnitudes was measured with a possible period of eight days.
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In July 2008, a rotational lightcurve of Elisa was obtained from photometric observations by Matthieu Conjat at Nice Observatory in France. Lightcurve analysis gave a well-defined rotation period of hours with a brightness variation of magnitude (). During the same opposition, Vladimir Benishek at Belgrade Observatory and Lucy Lim with the Spitzer-team determined a period for this asteroid of and hours with an amplitude of and magnitude, respectively ().
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At that distance, the visual magnitude is diminished by an extinction factor of 0.08 due to interstellar dust. This is a red giant star on the asymptotic giant branch, with a stellar classification of M2 III. It is a suspected variable star, although the evidence is considered "doubtful or erroneous". If it does exist, the variability is small with an amplitude of 0.05 magnitude and a timescale of around 30 days.
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In October 2005, a rotational lightcurve of Erna was obtained from photometric observations by French and Italian astronomers Raymond Poncy (), Roberto Crippa (), Federico Manzini and Silvano Casulli. Lightcurve analysis gave a well-defined rotation period of 8.7893 hours with a brightness variation of 0.35 magnitude (). Another lightcurve from the Palomar Transient Factory in November 2010 gave a similar period of 8.790 hours with an amplitude of 0.35 magnitude ().
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In November 2011, a rotational lightcurve of Frisia was obtained by astronomers at the University of North Dakota () and the Badlands Observatory in North Dakota, United States. Lightcurve analysis gave a rotation period of 14.557 hours with a brightness variation of 0.16 magnitude (). Photometric observations in the R-band at the Palomar Transient Factory in September 2011, gave a somewhat similar period of 18.500 hours and an amplitude of 0.15 magnitude ().
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In 2005, two rotational lightcurves of Gibbs were obtained from photometric observations by Italian amateur astronomers Federico Manzini and Roberto Crippa. Lightcurve analysis gave a rotation period of 3.06 and 3.06153 hours with a brightness variation of 0.31 and 0.39 magnitude, respectively (). In December 2016, Robert Stephens obtained a well-defined lightcurve at his Trojan Station () that gave a period of 3.189 hours and an amplitude of 0.26 magnitude ().
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Two rotational lightcurve of Gerti were obtained from photometric observations by Wiesław Wiśniewski in February 1988, and by astronomers at the Palomar Transient Factory in January 2011, respectively. Lightcurve analysis gave an identical rotation period of 3.082 hours with a respective brightness amplitude of 0.20 and 0.29 magnitude (). A third lightcurve by René Roy in March 2008 gave a period of 3.0 hours with an amplitude of 0.36 magnitude ().
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In February 1984, a rotational lightcurve of Gagarin obtained by American astronomer Richard P. Binzel gave a rotation period of 10.96 hours with a brightness variation of 0.24 magnitude (). Photometric observations at the Californian Palomar Transient Factory in December 2011, gave a 10.9430 hours with an amplitude of 0.41 (). in 2001 and 2016, additional lightcurve were obtained from modeled photometric data, giving a period of 10.94130 and 10.93791 hours ().
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In March 2011, a rotational lightcurve of Deira was obtained from photometric observations by Julian Oey at his Leura Observatory () in Australia. Lightcurve analysis gave a rotation period of 210.6 hours with a brightness variation of 0.5 magnitude (), while Oey previously published a slightly longer period of 217.1 hours and an amplitude of 0.6 magnitude (). This makes Deira one of the Top 300 slow rotators known to exist.
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In August 2005 and November 2012, two rotational lightcurves were obtained through photometric observations at the Chiro Observatory, Australia, and at the Preston Gott Observatory in Texas, United States, respectively. The ambiguous lightcurve from Chiro Observatory showed a rotation period of hours with a brightness variation of 0.35 in magnitude, when using the longer solution (). The other lightcurve at Preston Gott gave a period of hours with an amplitude of 0.23 ().
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A rotational lightcurve of Corbett was obtained from photometric observations by French amateur astronomer René Roy in July 2009. Lightcurve analysis gave a rotation period of 10 hours with a brightness amplitude of 0.12 magnitude (). Photometric observations in the R-band at the Palomar Transient Factory in 2010 and 2013, gave a divergent period of 11.453 () and 49.507 () hours with an amplitude of 0.19 and 0.10 magnitude, respectively.
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In October 2011, a rotational lightcurve of Beresford was obtained from photometric observations by Brian Skiff. Lightcurve analysis gave a rotation period of hours with a brightness variation of magnitude (), indicative of a spherical shape. The result supersedes an alternative period solution of hours (twice the period) with an amplitude of magnitude previously obtained by Robert A. Koff at the Antelope Hills Observatory in Colorado in October 2004 ().
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Several rotational lightcurves of Pori have been obtained from photometric observations since 2003. In August 2003, photometric observations made by Robert Stephens at the Santana Observatory () in California, gave a synodic rotation period of 3.36 hours. The lightcurve shows a brightness variation of 0.28 in magnitude (). In August 2016, another lightcurve by Maurice Audejean gave a refined rotation period of 3.3557 hours with an amplitude of 0.34 magnitude ().
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In June 1984, a first rotational lightcurve of Piccolo was obtained from photometric observations by American astronomer Richard Binzel. Lightcurve analysis gave a rotation period of 16.57 hours with a brightness variation of 0.33 magnitude (). In 2003 and 2005, two more lightcurves were obtained by French amateur astronomer René Roy. They gave a period of 16.048 and 16.05 hours and an amplitude of 0.24 and 0.29 magnitude, respectively ().
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In February 2013, a rotational lightcurve of Orsilocus was obtained from photometric observations by Robert Stephens at the Center for Solar System Studies (CS3) in Landers, California. Lightcurve analysis gave a rotation period of hours with a variation amplitude of 0.12 magnitude (). In 2015 and 2016, follow-up observations by Stephens at the CS3 gave two concurring periods of and hours with an amplitude of 0.20 and 0.16 magnitude, respectively ().
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It is a slowly pulsating B star with a frequency of 0.26877 d−1 and an amplitude of 0.0046 magnitude. The averaged quadratic field strength of the star's longitudinal magnetic field is . The star is around 32 million years old and is spinning rapidly with a projected rotational velocity of 264 km/s. It has an estimated 5.5 times the mass of the Sun and 3.8 times the Sun's radius.
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In December 1997, a rotational lightcurve of Luanda was obtained from photometric observations at the Félix Aguilar Observatory in Argentina . Lightcurve analysis gave a rotation period of 5.360 hours with a brightness variation of 1.0 magnitude (). In January 2007, French amateur astronomer René Roy obtained a period of 4.141 hours with an amplitude of 0.77 magnitude (). A high brightness amplitude indicates that the body has an elongated rather than spherical shape.
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In October 2015, a rotational lightcurve of Leonardo was obtained from photometric observations by astronomers at the University of Maryland using a 0.43-meter telescope at Mayhill, New Mexico . Lightcurve analysis gave a rotation period of hours with a brightness variation of 0.26 magnitude (). The result supersedes a tentative period determination by astronomers at Lindby Observatory which gave a spin rate of 8.54 and an amplitude of 0.20 magnitude ().
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During March and April 2013, photometric observations of Lagrula were made over ten nights by Italian astronomer Giovanni Casalnuovo at Eurac Observatory () in Bolzano, Italy. Lightcurve analysis gave a rotation period of 5.9176 hours and a brightness variation of 0.28 magnitude (). In January 2016, a more refined period of 5.882 hours with an amplitude of 0.44 magnitude was obtained from a bimodal lightcurve by Spanish astronomer group OBAS, Observadores de Asteroides ().
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In April 2015, a rotational lightcurve of Nicholson was obtained from photometric observations by a group of Spanish astronomers from Valencia and Alicante at various observatories: , , , and . Lightcurve analysis gave a well-defined rotation period of hours and a brightness variation of 0.24 magnitude (). At the same time, Serbian astronomer Vladimir Benishek at the Belgrade Observatory determined a concurring period of hours with an amplitude of 0.29 magnitude ().
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In September 1982, a first rotational lightcurve of Renzia was obtained from photometric observations at the Table Mountain Observatory in California. Lightcurve analysis gave a rotation period of 7.885 hours with a brightness variation of 0.42 magnitude (). In February 2012, observations in the R-band by astronomers at the Palomar Transient Factory gave an identical period with an amplitude of 0.49 magnitude (). Two 2016-studies also modeled the asteroid's lightcurve.
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Several rotational lightcurve for this asteroid were obtained from photometric observations since 1997. They gave a variety of rotation periods from 10.608 to 22.226 hours with inconsistent brightness variations in the range of 0.05 to 0.40 magnitude (). CALL adopts the results of the most observations made by astronomer Julian Oey at the Australian Blue Mountains Observatory in March 2014, which gave a period of hours and an amplitude of magnitude ().
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In May 2005, a rotational lightcurve of Cogshall was obtained from photometric observations by French amateur astronomer Pierre Antonini. Lightcurve analysis gave a well-defined rotation period of 3.62417 hours with a brightness variation of 0.21 magnitude (). Observations at the Palomar Transient Factory in 2012, gave a concurring period of 3.624 and 3.630 hours with an amplitude of 0.22 and 0.20 magnitude in the R- and S-band, respectively ().
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In May 2009, a rotational lightcurve of Beryl was obtained from photometric observations by Julian Oey at the Leura and Kingsgrove observatories in Australia. Lightcurve analysis gave a rotation period of hours and a brightness variation of 0.20 magnitude (). In addition, a nearly identical period of hours with an amplitude of 0.14 was determined in the R-band by astronomers at the Palomar Transient Factory in October 2010 ().
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At present it has 67 times the radius of the Sun. It is a variable star of uncertain type, changing brightness with an amplitude of 0.0058 in visual magnitude over a period of 8.5 days. The star radiates 927 times the luminosity of the Sun from its bloated photosphere at an effective temperature of 3,931 K. A magnitude 10 visual companion is located at an angular separation of .
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The Palomar Transient Factory in California obtained a rotational lightcurve of Menelaus from photometric observation in the R-band in October 2010. It gave a rotation period of 17.7390 hours with a brightness variation of 0.32 magnitude in the R-band (). In February 2014, a refined period of hours with an amplitude of 0.15 magnitude was determined by American astronomer Robert D. Stephens at the Center for Solar System Studies ().
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In March 2009, Czech astronomer Petr Pravec obtained a rotational light-curve from photometric observations at Ondřejov Observatory. It gave a well-defined rotation period of 9.6602 hours with a brightness variation of 0.55 magnitude (). One month later, a concurring period of 9.659 hours with an amplitude of 0.71 magnitude was obtained by Adrián Galád at Modra Observatory (). Photometric observations at the Palomar Transient Factory in December 2011.
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It is a Delta Scuti type variable star, with a dominant pulsation period of 0.1881 days and an amplitude of 0.016 in magnitude. David and Hillenbrand (2015) found an average mass for this star of 1.61 times the mass of the Sun, whereas Zorec and Royer (2012) list a much higher mass estimate of . It is about 356 million years old with a projected rotational velocity of 222 km/s.
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In September 1989, a rotational lightcurve of Brandia was obtained from photometric observations by American astronomer Richard Binzel at CTIO and McDonald Observatory. Lightcurve analysis gave a well-defined rotation period of hours with a relatively high brightness variation of 0.62 magnitude (). An identical period of 11.444 hours with an amplitude of 0.50 magnitude was measured with a Celestron 14-inch telescope by Frederick Pilcher and published in 1985 ().
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In December 2010, the best- rated rotational lightcurve of Lugduna was obtained from photometric observations by Gordon Gartrelle at the University of North Dakota and at the Badlands Observatory in South Dakota, United States. Analysis of the bimodal lightcurve gave a well-defined rotation period of 5.477 hours with a brightness variation of 0.43 magnitude (). Other observations gave a period of 5 and 5.478 hours with an amplitude of 0.33 ().
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In September 1989, the first rotational lightcurve of Wallenbergia was obtained from photometric observations by Polish astronomer Wiesław Z. Wiśniewski at University of Arizona. Lightcurve analysis gave a well-defined rotation period of 4.096 hours with a brightness amplitude of 0.33 magnitude (). Observations in the R-band at the Palomar Transient Factory in 2014, gave a period of 4.116 and 4.12 hours with an amplitude of 0.25 and 0.23 magnitude, respectively ().
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In March 1990, a rotational lightcurve of Dubiago was obtained using the Nordic Optical Telescope at the La Palma site on the Canary Islands. Lightcurve analysis gave a rotation period of 14.3 hours with a brightness variation of 0.23 magnitude (). A second lightcurve was obtained in the R-band at the Palomar Transient Factory in October 2013, giving an alternative period solution of 34.8374 hours with an amplitude of 0.21 magnitude ().
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In April 2005, a first rotational lightcurve of Christa was obtained from photometric observations by French amateur astronomers Raymond Poncy and René Roy. Lightcurve analysis gave a rotation period of 12.189 hours with a brightness variation of 0.20 magnitude (). In January 2009, a refined period of 11.230 hours and an amplitude of 0.12 magnitude was measured by photometrist Brian Warner at his Palmer Divide Observatory in Colorado, United States ().
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Photometric observations of Asta collected at the Australian Oakley Southern Sky Observatory and the U.S. Oakley Observatory in October 2008 show a rotation period of 7.99 hours with a brightness variation of 0.22 magnitude (). In February 2010, a refined lightcurve with a period of 7.554 hours and an amplitude of 0.14 magnitude was obtained by French amateur astronomer Pierre Antonini, who also mentioned the possibility of an alternative period solution ().
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In 2014, Pilcher revisited Paeonia at his Organ Mesa Observatory and measured a refined period of 7.9971 hours with an amplitude of 1.00 magnitude (), a strong indication for an elongated shape. A modeled lightcurve using photometric data from the Lowell Photometric Database was published in 2016. It gave an identical sidereal period of 7.9971 hours, as well as a spin axis at (155.0°, −50.0°) in ecliptic coordinates (λ, β).
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It is drifting further away with a radial velocity of +13 km/s. This star was originally thought to be a Beta Cephei variable and a suspected eclipsing binary with an orbital period of 133.92 days. It is now considered as probably constant. Measurements indicate that at most it is a microvariable star with an amplitude of 0.0041 in visual magnitude and a period of 0.42029 cycles per day.
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Methone's orbit is visibly affected by a perturbing 14:15 mean-longitude resonance with the much larger Mimas. This causes its osculating orbital elements to vary with an amplitude of about in semi-major axis, and 5° in longitude of its periapsis on a timescale of about 450 days. Its eccentricity also varies on different timescales between 0.0011 and 0.0037, and its inclination between about 0.003° and 0.020°.
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In January 2009, a rotational lightcurve of Saheki was obtained from photometric observations by David Higgins at Hunters Hill Observatory, Australia. Lightcurve analysis rendered a well-defined rotation period of hours with a brightness variation of 0.56 in magnitude (). Two months later, in March 2009, a second lightcurve was obtained at the Via Capote Observatory , California. It gave a period of and an amplitude of 0.68 in magnitude ().
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In November 2005, a rotational lightcurve of La Paz was obtained from photometric observations by French amateur astronomer René Roy. Lightcurve analysis gave a well-defined rotation period of 8.998 hours with a brightness amplitude of 0.14 magnitude (). In March 2007, a concurring period of 9.002 hours and an amplitude of 0.14 magnitude () was obtained by astronomers Roberto Crippa and Federico Manzini at the Sozzago Astronomical Station in Italy ().
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A rotational lightcurve of Ucclia was obtained from photometric observations by Italian and French astronomers Silvano Casulli, Federico Manzini and Pierre Antonini in March 2007. It showed a well-defined rotation period of hours with a brightness variation of 0.40 in magnitude (). In June 2008, a second light-curve by Slovak astronomer Adrián Galád at Modra Observatory, gave a concurring period of hours with an amplitude of 0.29 in magnitude ().
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The first rotational lightcurve was obtained by American astronomer Richard P. Binzel during a photometric survey of small main-belt asteroids in the 1980s. It showed a rotation period of 4.4 hours with a brightness variation of 0.09 magnitude (). In November 2004, another lightcurve of Kosmodemyanskaya was obtained by French amateur astronomer Laurent Bernasconi. Lightcurve analysis gave a period of 10 hours with an amplitude of 0.05 magnitude ().
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In June 2010, a rotational lightcurve of ' was obtained from photometric observations by Australian astronomers David Higgins and Julian Oey at the Hunters Hill and Leura Observatory . Lightcurve analysis gave a well-defined rotation period of hours with a brightness variation of 0.35 magnitude (). Several concurring period determinations in the range of 2.7091 to 2.710 hours with an amplitude of 0.26 to 0.36 magnitude were also made between 2007 and 2013 ().
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In December 2013, a rotational lightcurve of Franziska was obtained from photometric observations by American astronomer Frederick Pilcher at the Organ Mesa Observatory in New Mexico. Lightcurve analysis gave a well-defined rotation period of 16.507 hours with a brightness variation of 0.35 magnitude (). The result supersedes Richard Binzel's previously obtained lightcurve from May 1985, which gave a period of 14.0 hours and an amplitude of 0.53 magnitude ().
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In December 2015, a rotational lightcurve of Cydonia was obtained from photometric observations by astronomers at the Etscorn Observatory () in New Mexico, United States. Lightcurve analysis gave a well- defined rotation period of 2.679 hours with a brightness variation of 0.28 magnitude (). In April 2017, Spanish astronomers at Puçol Observatory () and other stations of the APTOG-network measured a similar period of 2.6700 hours and an amplitude of 0.10 magnitude ().
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In February 2020, a rotational lightcurve of Malzovia was obtained from photometric observations by French amateur astronomer René Roy. Lightcurve analysis gave a well-defined rotation period of () hours with a high brightness variation of magnitude, indicative of its elongated shape (). Alternative period determinations by Julian Oey and Frederick Pilcher in May 2014 gave very similar results of () and () hours, respectively, both with an amplitude of 0.30 magnitude ().
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In October 21010, a rotational lightcurve of Hanskya was obtained from photometric observations at the Sunflower Observatory in Kansas, United States . Lightcurve analysis gave a rotation period of 15.61 hours with a brightness amplitude of 0.18 magnitude (). More recent observations at the Palomar Transient Factory and by French amateur astronomer René Roy gave a longer period of 25.31 and 25.3481 hours and an amplitude of 0.38 and 0.25, respectively ().
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Between a quarter and a half of long period variables show very slow variations with an amplitude up to one magnitude at visual wavelengths, and a period around ten times the primary pulsation period. These are called long secondary periods. The causes of the long secondary periods are unknown. Binary interactions, dust formation, rotation, or non-radial oscillations have all been proposed as causes, but all have problems explaining the observations.
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San Diego is a slow rotator. In March 2005, a rotational lightcurve was obtained from photometric observations by American astronomer Brian Warner at his Palmer Divide Observatory () in Colorado. It gave a long rotation period of hours with a brightness variation of 0.60 in magnitude (). The period was derived from a re-examined lightcurve that originally gave a much shorter period of hours with an amplitude of 0.37 in magnitude ().
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HD 155035 is the Henry Draper Catalogue designation for a star in the constellation Ara, the Altar. It is located at a distance of approximately from Earth and has an apparent visual magnitude of 5.92, making it is faintly visible to the naked eye. This is a red giant star with a stellar classification of M1.5 III. It an irregular variable that changes brightness over an amplitude range of 0.12 magnitudes.
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This is a massive Be star with a stellar classification of B2Vne, where the 'n' indicates "nebulous" lines due to rapid rotation. It is spinning with a projected rotational velocity of 144 km/s. As the critical velocity for the star is 477 km/s, the inclination angle of its poles must be small; estimated as ~20°. It is a Gamma Cassiopeiae variable with an amplitude of 0.15 magnitude.
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Due to its constant phase with altitude, is most efficient to drive coherent winds at dynamo layer height,Kato, S., J. Geophys. Res., 71, 3211, 1966 while the currents generated by the internal modes interfere destructively at various heights.Forbes, J.M., J. Geophys.Res. 87, 5222, 1988 A Fourier analysis shows a semidiurnal component with an amplitude of 1 /2 of that of the diurnal component, phase shifted by 180°.
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A wavelet is a wave-like oscillation with an amplitude that starts out at zero, increases, and then decreases back to zero. It can typically be visualized as a "brief oscillation" that promptly decays. Wavelets can be used to extract information from many different kinds of data, including – but certainly not limited to – audio signals and images. Thus, wavelets are purposefully crafted to have specific properties that make them useful for signal processing.
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In October 2002, a rotational lightcurve of Annika was obtained from photometric observations by Colin Bembrick at Mount Tarana Observatory , Australia, in collaboration with Greg Bolt and Tom Richards near Perth and Melbourne, respectively. Lightcurve analysis gave a well-defined rotation period of hours with a brightness variation of magnitude (). This period was confirmed by Gérald Rousseau in March 2012, who determined a very similar period of hours with an amplitude of magnitude ().
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In February 2011, a rotational lightcurve of Walküre was obtained from photometric observations by astronomer Li Bin at the XuYi Station of the Purple Mountain Observatory in China. Lightcurve analysis gave a rotation period of hours with a brightness variation of magnitude, indicative of an elongated shape (). The result supersedes observations by Richard Binzel (1982) and René Roy (2005), who determined a period of and with an amplitude of and magnitude, respectively ().
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In August 2006, a rotational lightcurve of Athene was obtained from photometric observations by Roberto Crippa and Federico Manzini at the Sozzago Astronomical Station , Italy, and by Jean-Gabriel Bosch at the Collonges Observatory , France. Lightcurve analysis gave a rotation period of hours with a high brightness variation of magnitude, indicative of a non- spherical, elongated shape (). In September 2010, French amateur astronomer René Roy measured a similar period of hours and an amplitude of ().
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In April 2003, a rotational lightcurve of Imhilde was obtained from photometric observations by Brian Warner at the Palmer Divide Observatory in Colorado. In 2011, after more than a decade of additional experience in asteroid lightcurve photometry, Warner reexamined the data set using improved tools and techniques. Lightcurve analysis gave a rotation period of hours with a brightness variation of magnitude (). Originally, the same data gave a period of hours with an amplitude magnitude ().
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In March 2016, a rotational lightcurve of Whittemora was obtained from photometric observations by French and Swiss astronomers Christophe Demeautis, Mickael Porte and Raoul Behrend. Lightcurve analysis gave a rotation period of hours with a brightness variation of magnitude (). This result supersedes a period determination of 16+ hours by Pierre Antonini from June 2006 (), and of hours with an amplitude of magnitude by John Menke at the Menke Observatory in January 2004 ().
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In April 2010, a rotational lightcurve of Wallenquist obtained by American astronomer Robert Stephens at the Goat Mountain Astronomical Research Station (GMARS, ), California, gave a well-defined rotation period of hours with a brightness amplitude of 0.22 magnitude (). Two other observations, by French astronomer René Roy at Blauvac Observatory (), France, and by astronomers at the U.S. Palomar Transient Factory, gave a period of and , with an amplitude of 0.30 and 0.23, respectively ().
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After Piazzia had been published by The Minor Planet Bulletin as an opportunity for photometry in 2001, a classically shaped bimodal lightcurve was obtained by Robert Stephens at the Santana Observatory in Rancho Cucamonga, California. The lightcurve gave a rotation period of hours with a brightness variation of 0.45 magnitude (). A second lightcurve was obtained by astronomer René Roy in March 2007, rendering a period of hours and an amplitude of 0.2 magnitude ().
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In August 2004, a rotational lightcurve of Martina was obtained from photometric observations by David Higgins at the Hunters Hill Observatory in Australia. Lightcurve analysis gave a rotation period of hours with a brightness variation of magnitude (). Astronomers at the Palomar Transient Factory in California also determined the period in the R-band on two occasions, measuring 11.263 and 11.268 hours with an amplitude of 0.24 and 0.15 in 2010 and 2012, respectively ().
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It is a Mira-type long period variable that varies by an amplitude of 4.27 in visual magnitude over a period of . Evidence has been found of asymmetry in this star, suggesting a non-spherical shape. Abundance-wise, it is an oxygen-rich giant and the emission feature is of the oxygen-rich silicate class as it sheds silicate dust from its atmosphere. The star is shedding mass at the rate of ·yr−1.
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161 Athor is an M-type Main belt asteroid that was discovered by James Craig Watson on April 19, 1876, at the Detroit Observatory and named after Hathor, an Egyptian fertility goddess. An occultation by Athor was observed, on October 15, 2002, resulting in an estimated diameter of . Photometric observations of the minor planet in 2010 gave a rotation period of with an amplitude of in magnitude. This result is consistent with previous determinations.
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Additionally, the emitted sound from the instrument was recorded, under controlled conditions, and spectrally analyzed. Major findings include the concentration of the emitted sound between 400 Hz and 800 Hz, with an amplitude modified in a manner consistent with the experimentally measured vibrational characteristics of the instrument’s sound box and bridge. The experimental results validate the historical evidence that chelys was used in Greek antiquity as an accompaniment instrument to the human voice.
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In October 2007, a rotational lightcurve of Jeanperrin was obtained from photometric observations by a large international collaboration of astronomers. Lightcurve analysis gave a rotation period of 3.6169 hours and a low brightness variation of 0.09 magnitude, indicative of a nearly spheroidal shape (). Additional observations by Petr Pravec at Ondřejov Observatory in 2007 and 2017, rendered a nearly identical period of 3.6169 and 3.61692 hours with an amplitude of 0.09 and 0.10 magnitude, respectively ().
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As of 2017, no secure rotational lightcurve of Henan has been obtained. In September 2004, observations by Laurent Bernasconi gave a rotation period of 24 hours with a brightness variation of 0.25 magnitude (). In February 2015, photometric observations of Henan by an international collaboration of astronomers gave a tentative synodic period of hours and an amplitude of 0.4 magnitude, which would make it a potentially slow rotator (). An alternative period solution gave 94 hours.
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In September 1996, photometric observations of Halaesus were made by Italian astronomer Stefano Mottola, using the now decommissioned Bochum 0.61-metre Telescope at ESO's La Silla Observatory in Chile. The resulting rotational lightcurve showed a well- defined period of hours with a brightness variation of in magnitude (). In August 2015, observations by the Kepler space telescope gave two period determinations of 25.052 and 29.95 hours with an amplitude of 0.23 and 0.19 magnitude, respectively ().
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A rotational lightcurve of this asteroid was obtained from photometric observations made by Czech astronomer Petr Pravec at the Ondřejov Observatory in August 2014. The lightcurve gave a well-defined rotation period of hours with a brightness variation of 0.27 in magnitude (). One month later, in September 2014, a second lightcurve by American astronomer Brian Warner at his Palmer Divide Observatory, Colorado, gave a concurring period of hours with an amplitude of 0.23 in magnitude ().
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In the early 1980s, a rotational lightcurve of Galanthus was obtained during a survey conducted by Richard P. Binzel at the McDonald Observatory, Texas. Lightcurve analysis gave a well-defined rotation period of 3.92 hours with a brightness variation of 0.28 magnitude (). The period was confirmed from photometric observations by astronomers at the Palomar Transient Factory in October 2015, which gave a similar period of 3.918 hours and an amplitude of 0.22 magnitude ().
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In April 2011, a rotational lightcurve of Houston was obtained from photometric observations by astronomers at the Oakley Southern Sky Observatory () in Australia. Lightcurve analysis gave a well-defined rotation period of 11.218 hours with a brightness amplitude of 0.11 magnitude (). Two more lightcurves obtained at the Palomar Transient Factory in 2014, gave a period of 5.61 (half the period solution) and 11.175 hours with an amplitude of 0.17 and 0.14 magnitude, respectively ().
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In March 2007, a rotational lightcurve of Duponta was obtained from photometric observations by a collaboration of Czech (Ondřejov Observatory), Slovak (Modra Observatory), Australian and American astronomers. Lightcurve analysis gave a well-defined rotation period of 3.85453 hours with a brightness variation of 0.23 magnitude (). Follow-up observations by Petr Pravec in 2007 and 2010, gave a concurring period of 3.85449 and 3.85453 hours with an amplitude of 0.26 and 0.23 magnitude, respectively ().
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A two chord stellar occultation by the asteroid observed in 2004 gave an approximate diameter of 50 km. French amateur astronomer Pierre Antonini obtained a lightcurve of Dufour from photometric observations taken during April 2010. Lightcurve analysis gave a well-defined rotation period of hours with an amplitude of 0.31 in magnitude (). In August 2013, photometric observations at the Palomar Transient Factory, California, gave a similar period of hours with a brightness variation of 0.35 ().
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In September 2012, a rotational lightcurve of Aretaon was obtained from photometric observations by Robert Stephens at the Center for Solar System Studies in Landers, California. Lightcurve analysis gave a rotation period of 8.05 hours with a brightness amplitude of 0.17 magnitude (). This period determination was confirmed by astronomers at the Palomar Transient Factory in September 2013, measuring a period of 8.048 hours and an amplitude of 0.19 magnitude in the R-band ().
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In November and December 2002, two rotational lightcurves of Cimbria were obtained from photometric observations by Italian amateur astronomers Silvano Casulli, Antonio Vagnozzi, Marco Cristofanelli and Marco Paiella. Lightcurve analysis gave a well-defined rotation period of 5.65 hours with a brightness variation of 0.40 and 0.57 magnitude, respectively (). In December 2012, astronomers at the Palomar Transient Factory in California measured a period of 5.655 hours and an amplitude of 0.26 magnitude ().
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In 1998, a rotational lightcurve of Poseidon was published from photometric observations made by Czech astronomer Petr Pravec at Ondřejov Observatory. It gave a period of hours with a brightness variation of 0.08 magnitude (). A second lightcurve was obtained during the Near-Earth Objects Follow-up Program which gave a concurring period of hours and an amplitude of 0.07 magnitude (). A low brightness variation typically indicates that the body has a nearly spheroidal shape.
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In July 2010, a rotational lightcurve of Palinurus was obtained during eight consecutive nights by Italian astronomer Stefano Mottola at the Calar Alto Observatory in Spain. Lightcurve analysis gave a rotation period of hours with a brightness variation of 0.09 magnitude (). In January 2015, photometric observations by Robert Stephens at the Center for Solar System Studies in Landers, California, determined a period of hours with an amplitude of 0.16 magnitude based on a fragmentary lightcurve ().
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In October 1989, a rotational lightcurve of Peiroos was obtained from photometric observations by German and Italian astronomers. Lightcurve analysis gave a well-defined rotation period of 8.96 hours with a brightness variation of 0.30 magnitude (). Between 2015 and 2017, photometric observations by Robert Stephens and collaborators at the Center for Solar System Studies in Landers, California, gave two concurring periods of 8.951 and 8.99 hours, both with an amplitude of 0.31 magnitude ().
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In February 2008, a rotational lightcurve of Perth was obtained by a collaboration of astronomers in a photometric survey of the Flora region. Lightcurve analysis gave a rotation period of 5.083 hours with a brightness variation of 0.28 magnitude (). Other photometric observations at the Palomar Transient Factory in October 2010, and by Wiesław Wiśniewski in December 1993, gave a period of 5.087 and 5.2 hours with an amplitude of 0.92 and 1.09, respectively ().
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In February 2008, a rotational lightcurve of Luthera was obtained from photometric observations by Mexican astronomer Pedro Sada at the University of Monterrey, Mexico. Lightcurve analysis gave a short rotation period of 5.878 hours with a low brightness variation of 0.05 magnitude, indicative for a nearly spherical shape (). A lower-rated lightcurve with a period of 7.92 hours and an amplitude of 0.06 magnitude was obtained by French amateur astronomer Pierre Antonini in May 2009 ().
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Lappeenranta has an ambiguous rotation period. Recent photometric observations gave a period of 15.16 and 15.190 hours with a brightness variation of 0.09 and 0.22 magnitude, respectively (), while Richard Binzel obtained a period of 10.44 hours and an amplitude of 0.29 magnitude in the mid-1980s (). An alternative period of 8 hours, which was measured by Laurent Bernasconi and Fernand van den Abbeel (2002) as well as by René Roy (2006), has been superseded ().
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In November 2011, a rotational lightcurve of Moffatt was obtained from photometric observations by Chinese astronomers using the SARA telescopes of the Southeastern Association for Research in Astronomy at Kitt Peak and CTIO. Lightcurve analysis gave a rotation period of 5.187 hours and a brightness variation of 0.12 magnitude (). This supersedes a previous result from a fragmentary lightcurve by that gave a period of 5.195 hours with an amplitude of 0.27 magnitude ().
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So in oscillators that must produce a very low-distortion sine wave, a system that keeps the gain roughly constant during the entire cycle is used. A common design uses an incandescent lamp or a thermistor in the feedback circuit., "Alternatively, an amplitude-controlled resistor or other passive nonlinear element may be included as part of the amplifier or in the frequency-determining network.", Amplitude of Oscillation—Part II, Automatic Gain Control.
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It is thought to have been ejected from the OB association Sco OB 1 approximately 14 million years ago. The primary component is a B-type main-sequence star with a stellar classification of B2V. It displays microvariability with an amplitude of 0.0086 in magnitude and a frequency of 0.11316 cycles per day. The star is an estimated 14 million years old with a high rate of spin, showing a projected rotational velocity of 122.
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In September 2001, a rotational lightcurve of Stavropolis was obtained from photometric observations by Americans Larry Robinson and Brian Warner at the Sunflower and Palmer Divide Observatory in Kansas and Colorado, respectively. Lightcurve analysis gave a rotation period of hours with a brightness variation of 0.42 magnitude (). In October 2015, another lightcurve was obtained by French amateur astronomer Pierre Antonini. It gave a well- defined period of hours with an amplitude of 0.32 magnitude ().
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In April 2007, a rotational lightcurve of Saskia was obtained from photometric observations by French amateur astronomer Pierre Antonini. Lightcurve analysis gave a well-defined rotation period of hours with a brightness variation of 0.36 magnitude (). In December 2016, an identical period with an amplitude of 0.28 magnitude was determined by Daniel Klinglesmith at Etscorn Campus Observatory , New Mexico (). This result supersedes two previous observations that gave a period of 7.34 and 7.349 hours, respectively ().
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Estimated to be around 10 billion years old, this is an aging red giant star with a stellar classification of M3.5 III. It is a periodic variable with a frequency of 11.98912 cycles per day and an amplitude of 0.0254 in magnitude. The spectrum does not show evidence of s-process enhancement. 10 Dra has 93% of the mass of the Sun but has expanded to about 83 times the Sun's radius.
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HD 83944 is a star system in the constellation Carina. This has the Bayer designation m Carinae, while HD 83944 is the identifier from the Henry Draper catalogue. It is a suspected variable with an apparent visual magnitude that fluctuates around 4.51 with an amplitude of 0.5. The system is located at a distance of approximately 226 light years from the Sun based on parallax, and it has an absolute magnitude of 0.31.
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Hurricane Wilma on 19 October 2005; in the storm's eye Atmospheric pressure varies widely on Earth, and these changes are important in studying weather and climate. See pressure system for the effects of air pressure variations on weather. Atmospheric pressure shows a diurnal or semidiurnal (twice-daily) cycle caused by global atmospheric tides. This effect is strongest in tropical zones, with an amplitude of a few millibars, and almost zero in polar areas.
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Pallene is visibly affected by a perturbing mean-longitude resonance with the much larger Enceladus, although this effect is not as large as Mimas's perturbations on Methone. The perturbations cause Pallene's osculating orbital elements to vary with an amplitude of about 4 km in semi-major axis, and 0.02° in longitude (corresponding to about 75 km). Eccentricity also changes on various timescales between 0.002 and 0.006, and inclination between about 0.178° and 0.184°.
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In October 2005, a rotational lightcurve of Sekiguchi was obtained from photometric observations by French amateur astronomers René Roy and Laurent Bernasconi. Lightcurve analysis gave a well-defined rotation period of hours with a brightness variation of 0.72 magnitude (). In October 2010 and November 2011, two more lightcurves were obtained at the Palomar Transient Factory, rendering a period of 5.4048 and 5.4100 hours with an amplitude of 0.58 and 0.27 magnitude, respectively ().
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BB Phoenicis is a variable star in the constellation of Phoenix. It has an average visual apparent magnitude of 6.17, being visible to the naked eye with excellent viewing conditions. From parallax measurements by the Gaia spacecraft, it is located at a distance of from Earth. Its absolute magnitude is calculated at 0.6. BB Phoenicis is a Delta Scuti variable, and shows stellar pulsations that cause brightness variations with an amplitude of 0.04 magnitudes.
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In August 2006, a rotational lightcurve of Savo was obtained from photometric observations by Czech astronomer Petr Pravec at Ondřejov Observatory. Lightcurve analysis gave a well-defined rotation period of 5.35011 hours with a brightness amplitude of 0.52 magnitude (), indicative for a non-spherical shape. Follow up observations at the Calvin College Observatory () in 2007 and 2008, gave three nearly identical periods of 5.35020, 5.35031 and 5.35062 hours with an amplitude between 0.44 and 0.63 ().
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In May 2011, photometric observation of Lobachevskij gave a rotation period of 5.413 and 5.435 hours with a brightness amplitude of 0.30 and 0.33 magnitude, respectively (), superseding a previous period of 7.00 hours (). In September 2012, two rotational lightcurves were obtained in the S- and R-band at the Palomar Transient Factory in California. Lightcurve analysis gave a period of 5.409 and 5.4141 hours with an amplitude of 0.26 and 0.22 magnitude, respectively ().
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In September 2011, a rotational lightcurve of Carla was obtained from photometric observations by astronomer Frederick Pilcher at Organ Mesa Observatory near Las Cruces, New Mexico. Lightcurve analysis gave a rotation period of 6.1514 hours with a brightness amplitude of 0.25 magnitude (). in 2014, two additional lightcurves in the R-band, obtained at the Palomar Transient Factory, California, gave a period of 6.15 and 6.154 hours with an amplitude of 0.24 and 0.25, respectively ().
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During Pray's photometric observations, it was revealed that Zech (primary) is in fact an asynchronous binary asteroid with a minor planet moon orbiting it. The moon has an orbital period of 117.2 hours and a spin rate of 18.718 hours with an amplitude 0.08 magnitude. Based on Pray's secondary-to- primary mean diameter ratio (Ds/p) of more than 0.29, the Johnston's Archive estimates a diameter of at least 2.21 kilometers for Zechs companion.
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In March 2004, a rotational lightcurve of Zeelandia was obtained from photometric observations by a collaboration of American astronomers. Lightcurve analysis gave a well-defined rotation period of 15.602 hours with a brightness variation of 0.61 magnitude (). The result was confirmed by photometrists Pierre Antonini, Federico Manzini, Julian Oey and Frederick Pilcher, as well as Hiromi and Hiroko Hamanowa, who measured a similar period of 15.624 with an amplitude of 0.50 magnitude in April 2005 ().
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HD 28185 b was discovered by detecting small periodic variations in the radial velocity of its parent star caused by the gravitational attraction of the planet. This was achieved by measuring the Doppler shift of the star's spectrum. In 2001 it was announced that HD 28185 exhibited a wobble along the line-of-sight with a period of 383 days, with an amplitude indicating a minimum mass 5.72 times that of Jupiter.
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The downlink uses an amplitude modulation on the 27.095 MHz frequency. This frequency is used to power the passive balises (it is the intermediate channel 11A in CB radio). The uplink uses frequency-shift keying with 3.951 MHz for a logical '0' and 4.516 MHz for a logical '1'. The data rate of 564.48 kBit/s is enough to transmit 3 copies of a telegram to a train passing at 500 km/h.
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Modern studies show a smaller amplitude, with some showing almost no variation. Hipparcos photometry shows an amplitude of only about 0.02 magnitudes and a possible period around 18 days. Intensive ground-based photometry showed variations of up to 0.03 magnitudes and a possible period around 91 days. Analysis of observations over a much longer period still find a total amplitude likely to be less than 0.1 magnitudes, and the variation is considered to be irregular.
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They typically have a response latency of no more than six milliseconds with an amplitude of approximately one microvolt. The latency of the responses gives critical information: if cortical deafness is applicable, LLR (long-latency responses) are completely abolished and MLR (middle latency responses) are either abolished or significantly impaired. In auditory agnosia, LLRs and MLRs are preserved. Another important aspect of cortical deafness that is often overlooked is that patients feel deaf.
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We are able to use the action of the Hamiltonian constraint on the vertex of a spin network state to associate an amplitude to each "interaction" (in analogy to Feynman diagrams). See figure below. This opens up a way of trying to directly link canonical LQG to a path integral description. Now just as a spin networks describe quantum space, each configuration contributing to these path integrals, or sums over history, describe 'quantum space-time'.
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This raises philosophical problems: suppose that random physical processes happen on length scales both smaller than and bigger than the particle horizon. A physical process (such as an amplitude of a primordial perturbation in density) that happens on the horizon scale only gives us one observable realization. A physical process on a larger scale gives us zero observable realizations. A physical process on a slightly smaller scale gives us a small number of realizations.
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Between April 2008 and June 2015, five rotational lightcurves were obtained from photometric observations by Czech astronomer Petr Pravec at the Ondřejov Observatory near Prague. All lightcurves show a well-defined rotation period between 3.548 and 3.550 hours with a brightness variation of 0.15 to 0.18 in magnitude (). In April 2008, a photometric observation by astronomer Julian Oey at the Kingsgrove Observatory, Australia, gave a concurring period of hours and an amplitude of 0.14 ().
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In September 2007, a rotational light-curve of Lemaître was obtained from photometric observations by American astronomer Brian D. Warner at his Palmer Divide Observatory, Colorado. It gave a rotation period of 11.403 hours with a brightness variation of 0.04 magnitude (), superseding a provisional period of 2.4 hours with an amplitude of 0.03 magnitude, derived from photometric observations made by Arnaud Leroy, Bernard Trégon, Xavier Durivaud and Federico Manzini two months earlier ().
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In January 2012, a rotational lightcurve of Mason–Dixon was obtained from photometric observations by astronomers at the Palomar Transient Factory in California. Lightcurve analysis gave a rotation period of hours with a high brightness variation of 0.70 magnitude (), indicative of an elongated, non-spherical shape. Another fragmentary lightcurve by Maurice Clark at Preston Gott Observatory in September 2014 gave a less accurate period of 10.20 hours with an amplitude of 0.75 magnitude.
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In late 1988, a rotational lightcurve of Faïna was obtained from photometric observations by Richard Miles at the Manley Observatory near Chester in northwest England. Lightcurve analysis gave a well-defined rotation period of hours with a brightness variation of magnitude (). Alternative observations by Roberto Crippa, Federico Manzini (2006) as well as by Bruno Christmann (2019) determined a period of + and () hours (or half the period) with an amplitude of and magnitude ().
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In September 1981, a rotational lightcurve of Marlu was obtained from photometric observations by American astronomer Alan W. Harris. Lightcurve analysis gave a rotation period of hours with a brightness variation of magnitude (). In October 2014, Daniel A. Klinglesmith confirmed the exact same period of () hours with an amplitude of () magnitude (). In 2016, a modeled lightcurve gave a concurring sidereal period of hours using data from a large collaboration of individual observers.
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In May 2009, a rotational lightcurve of Berkeley was obtained from photometric observations by American amateur astronomer Joe Garlitz at his Elgin Observatory in Oregon. Lightcurve analysis gave a rotation period of hours with a brightness variation of magnitude (). Lower rated lightcurves obtained by Claes-Ingvar Lagerkvist in 1977, and by David Romeuf in 2018, gave a divergent period of larger than and with an amplitude of larger than and magnitude, respectively ().
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This is a B-type subgiant star with a stellar classification of B2 IV. It was determined to be a Beta Cephei variable based on observations during 1955 at the Cape Observatory. Tau1 Lupi shows a steady period of 0.17736934 days, corresponding to a frequency of 5.637953 cycles per day, with an amplitude of 0.035 in visual magnitude. It has around 10 times the mass of the Sun and 7 times the Sun's radius.
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In 2014, two rotational lightcurves of were obtained from photometric observations by American astronomer Brian Warner at the CS3–Palmer Divide Station in California (). Lightcurve analysis gave a rotation period of 5.370 and 5.66 hours and a brightness variation of 0.18 and 0.06 magnitude, respectively (), one of which gave an alternative period solution of hours. In April 2016, the EURONEAR lightcurve survey measured a period of 5.398 hours with an amplitude of 0.12 magnitude ().
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A wavelet is a wave-like oscillation with an amplitude that begins at zero, increases, and then decreases back to zero. It can typically be visualized as a "brief oscillation" like one recorded by a seismograph or heart monitor. Generally, wavelets are intentionally crafted to have specific properties that make them useful for signal processing. Using convolution, wavelets can be combined with known portions of a damaged signal to extract information from the unknown portions.
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Tombstone in Olynthus The classical city was established on the much larger north hill and to its eastern slope. The excavations, which cover only 1/10 of the city's total area, have revealed a Hippodamian grid plan. Two large avenues were discovered, with an amplitude of 7 meters, along with vertical and horizontal streets that divided the urban area into city blocks. Each one had ten houses with two floors and a paved yard.
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476Cruft Electronics Staff, p. 679. The dc grid voltage will vary with the modulation envelope of an amplitude modulated signalCruft Electronics Staff, p. 681. The plate current is passed through a load impedance chosen to produce the desired amplification in conjunction with the tube characteristics. In non-regenerative receivers, a capacitor of low impedance at the carrier frequency is connected from the plate to cathode to prevent amplification of the carrier frequencyK.
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The stellar classification is A3p SrCr, where the suffix notation indicates abundance anomalies of the iron-peak element chromium, as well as strontium. This is an Alpha2 Canum Venaticorum (ACV) variable, which indicates it varies in luminosity as it rotates due to spots on its surface created by a magnetic field. The range of variation has an amplitude of 0.02 magnitude and a period of just over two days. Samus et al.
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In 1969, γ Coronae Borealis was confirmed to be variable with an amplitude of 0.05 magnitudes. A year later, it was "confirmed" to be a δ Scuti variable with the earliest known spectral type in the class. The observed variations were not strictly periodic, but showed a characteristic timescale of 0.03 days (43 minutes). γ Coronae Borealis also showed anomalous behaviour not seen in other δ Scuti stars, such as periods without variation.
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It is a semiregular variable star of subtype SRb, ranging in magnitude from 4.28 down to 4.36. The star has pulsation periods of 18.8 and 45.5 days, each with an amplitude of 0.019 in magnitude. With the hydrogen at its core exhausted, the star has expanded to around 69 times the Sun's radius and it is radiating 1,021 times the luminosity of the Sun from its swollen photosphere at an effective temperature of 3,915 K.
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The companion has been identified from a high excitation component in the spectrum and from radial velocity variations, but the orbit is unknown. U Lacertae is a variable star classified as a semiregular variable. The periodicity is uncertain but a main period of 150 days and a long secondary period of 550 – 690 days have been suggested. A study of Hipparcos satellite photometry found an amplitude of 0.77 magnitudes and found no periodicity.
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In January 2005, a rotational lightcurve of Franklin-Adams was obtained from photometric observations by French amateur astronomer René Roy. Lightcurve analysis gave a rotation period of 3.082 hours with a brightness amplitude of 0.23 magnitude (). In March 2010, photometry at the Palomar Transient Factory in California gave a period of 2.979 with an amplitude of 0.32 magnitude (). In January 2013, American astronomer Brian Warner obtained the so-far best rated lightcurve.
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This is a magnetic, helium- weak Bp star with a stellar classification of B8 IIImnp. It is sometimes classified as a mercury-manganese star. It is also an 'sn' star, displaying a spectrum with generally sharp lines for most elements in combination with broad, diffuse lines of helium. 36 Lyncis has been classified as an SX Arietis variable with an amplitude of 0.03 in visual magnitude and a rotationally- modulated period of 3.834 days.
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The output of an ideal polarizer is a specific polarization state (usually linear polarization) with an amplitude equal to the input wave's original amplitude in that polarization mode. Power in the other polarization mode is eliminated. Thus if unpolarized light is passed through an ideal polarizer (where g1=1 and g2=0) exactly half of its initial power is retained. Practical polarizers, especially inexpensive sheet polarizers, have additional loss so that g1 < 1\.
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There are two opposing conventions for the representations of data. The first of these was first published by G. E. Thomas in 1949 and is followed by numerous authors (e.g., Andy Tanenbaum). It specifies that for a 0 bit the signal levels will be low-high (assuming an amplitude physical encoding of the data) - with a low level in the first half of the bit period, and a high level in the second half.
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Given its distance of about , the star is more than three times the distance from the Sun than Regulus. At this distance, the visual magnitude of Epsilon Leonis is reduced by 0.03 as a result of extinction caused by intervening gas and dust. Epsilon Leonis exhibits the characteristics of a Cepheid-like variable, changing by an amplitude of 0.3 magnitude every few days. It has around four times the mass of the Sun and a projected rotational velocity of .
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In 1983, a rotational lightcurve of Tauris, obtained from photometric observations with the ESO 0.5-metre telescope at La Silla, Chile, was by published by Belgian astronomer Henri Debehogne in collaboration with Italian astronomers Giovanni de Sanctis and Vincenzo Zappalà. Lightcurve analysis gave a rotation period of hours with a brightness variation of magnitude (). In May 2013, Michael S. Alkema at the Elephant Head Observatory in Arizona determined an identical period of hours with an amplitude of magnitude ().
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815 Coppelia is a minor planet orbiting the Sun that was discovered by German astronomer Max Wolf on 2 February 1916 from Heidelberg named after Coppélia, a comic ballet. Photometric observations of this asteroid at the Rozhen Observatory in Bulgaria during 2010 gave a light curve with a period of 4.4565 hours and a brightness variation of 0.24 in magnitude. This is consistent with a period of 4.421 hours and an amplitude of 0.27 obtained during a 2006 study.
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In September 2017, a rotational lightcurve of Swetlana was obtained from photometric observations by Thomas A. Polakis at the Command Module Observatory in Arizona. Lightcurve analysis gave a well-defined rotation period of hours with a brightness variation of magnitude (). The result supersedes an observations by Italian amateur astronomers Roberto Crippa and Federico Manzini at the Sozzago Astronomical Station from September 2006, which tentatively determined a period of more than 20 hours and an amplitude of magnitude ().
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Over the course of seven nights in January 2018, a rotational lightcurve of Ratisbona was obtained from photometric observations by Tom Polakis at the Command Module Observatory in Arizona. Lightcurve analysis gave a rotation period of hours with a low brightness variation of magnitude, indicative of a regular, spherical shape (). The result supersedes a period of hours with an amplitude of magnitude determined by René Roy, Raoul Behrend, Pierre Antonini and Donn Starkey in October 2004 ().
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In September 2016, a rotational lightcurve of Hel was obtained from photometric observations by Pedro Brines and colleges of the Spanish group of asteroid observers (OBAS). Lightcurve analysis gave a rotation period of hours with a brightness variation of magnitude (). The result supersedes previous observations by French amateur astronomers Laurent Bernasconi and René Roy in December 2001 and February 2004, which gave two tentative periods of and hours with an amplitude of 0.12 and 0.14, respectively.
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It showed a period of hours with an amplitude of magnitude (). The overall amplitude suggest a rather regular shape with a ratio of 0.86 for the length of the a and b axes. In 2018, Czech astronomers Josef Ďurech and Josef Hanuš published a modeled lightcurve using photometric data from the Gaia probe's second data release. It showed a sidereal period of hours, and gave a spin axis at (354.0°, 80.0°) in ecliptic coordinates (λ, β).
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In March 2009, a rotational lightcurve of Buda was obtained from photometric observations by Brian Warner at his Palmer Divide Observatory in Colorado. Analysis gave a classically shaped bimodal lightcurve with a rotation period of hours and a brightness variation of magnitude (). This supersedes a period determination by French amateur astronomer Laurent Bernasconi from January 2005, who determined a period of hours with an amplitude of magnitude (). Observations by Julian Oey in 2015 gave two similar periods ().
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3D-model of Kunigunde based on its lightcurve In March 2018, a rotational lightcurve of Kunigunde was obtained from photometric observations by French amateur astronomer René Roy. Lightcurve analysis gave a well-defined rotation period of hours with a brightness variation of magnitude (). Richard Ditteon at the Oakley Southern Sky Observatory determined a period of with an amplitude of magnitude (). Photometry by Angeli and Guimarães at observatories in Brazil and Argentina gave a similar period of hours ().
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In June 2015, a rotational lightcurve was obtained for this asteroid from photometric observations by astronomer Daniel Klinglesmith at Etscorn Campus Observatory , New Mexico. Lightcurve analysis gave a rotation period of hours with a brightness variation of 0.55 in magnitude (), indicative of a non-spherical, elongated shape. Previously, in August 2012, a concurring period of hours with an amplitude of 0.46 was determined from observations in the R-band by astronomers at the Palomar Transient Factory, California ().
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The star is classed as a cool semiregular variable of type SRc with a pulsational period of 732 days. The variations sometimes have an amplitude comparable to a long period variable, at other times they are much smaller. The spectral type varies between M4e around visual maximum and M9.8e at minimum light, and the luminosity class is Ia indicating a bright supergiant. The spectrum shows emission lines indicating that the star is losing mass through a strong stellar wind.
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The suffix notation indicates abundance anomalies of silicon, strontium, and mercury in the spectrum. It is an α2 Canum Venaticorum variable with an amplitude of 0.05 magnitude in the B (blue) band. The star is rotating slowly with a projected rotational velocity of 4.5 km/s. It is radiating 139 times the luminosity of the Sun from its photosphere at an effective temperature of 10,307 K. The secondary component has been reported to have characteristics of an Am star.
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In July 2008, American astronomer Brian Warner obtained a rotational lightcurve of Imatra at his Palmer Divide Observatory in Colorado. It gave a rotation period of 18.635 hours with a brightness variation of 0.28 magnitude (), superseding a period of 5.23 hours from observations at Italian and French observatories in the 1990s (). In September 2014, photometric observations by French amateur astronomers Laurent Bernasconi, Romain Montaigut and Arnaud Leroy gave a period of 18.609 hours with an amplitude of 0.27 magnitude ().
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In April 2016, a rotational lightcurve of Gordonmoore was obtained from photometric observations by astronomer Brian Warner at the Palmer Divide Station () in Colorado. It gave a rotation period of hours with a brightness variation of 0.25 magnitude. Lightcurve analysis also gave an alternative period solution of 4.19 hours with an amplitude of 0.25 magnitude. (). The results supersede a previous observations made at the Hoher List Observatory in Germany, that gave a shorter period of 6 hours ().
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In August 2017, a rotational lightcurve of Argelander was obtained from photometric observations at the Chilean Cerro Tololo Inter-American Observatory using the SARA South Telescope. Lightcurve analysis gave a rotation period of hours and a brightness variation of 0.48 magnitude (). In January 2012, astronomers at the Palomar Transient Factory had also determined a period of with an amplitude of 0.41 magnitude (). A modeled lightcurve using photometric data from the Lowell Photometric Database was published in 2016.
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The measured angular diameter, after correction for limb darkening, is . At the estimated distance of the star, this yields a physical size of about 67 times the radius of the Sun. It is a suspected variable star, with an amplitude of 0.01 magnitude. The star radiates 864 times the solar luminosity from its outer atmosphere with an effective temperature of 4,053 K. In the next 7500 years, the south Celestial pole will pass close to this stars (4200 CE).
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It has a well-defined rotation period of 2.98 hours, derived from two rotational lightcurve analysis. In March 2004, photometric observations at the U.S. Magdalena Ridge Observatory in New Mexico rendered a period of 2.980 hours with a brightness variation of 0.20 in magnitude (). In 2008 a second, concurring period was obtained by French amateur astronomer Pierre Antonini at his private Observatoire de Bédoin in France (). It gave a period of 2.9887 hours and an amplitude 0.22 in magnitude ().
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Between 2008 and 2011, three rotational lightcurves of Knushevia were obtained from photometric observations by American astronomer Brian Warner. Lightcurve analysis gave a rotation period between 4.45 and 4.717 hours with an exceptionally low brightness amplitude of 0.01 magnitude (). In May 2015, Warner measured a period of 3.1422 hours with an amplitude of 0.09 (). The photometric observation also revealed that Knushevia might be a binary asteroid with a minor-planet moon orbiting it every 11.922 hours.
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In September 1991, a first rotational lightcurve of Krok was obtained by American astronomer Alan Harris. Lightcurve analysis gave an exceptionally long rotation period of 147.8 hours with a brightness amplitude of 1.0 magnitude, which indicates that the body has a non-spheroidal shape (). Between 2000 and 2005, several photometric observations made by Czech astronomer Petr Pravec gave a similar period between 149.4 and 151.8 and an amplitude of 0.7 to 1.3 (). This makes Krok as slow rotator.
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In August 2013, a rotational lightcurve of Lujiaxi was obtained from photometric observations by Italian amateur astronomer Silvano Casulli. Lightcurve analysis gave a rotation period of 10.415 hours (given as 0.43397 days) with a brightness amplitude of 0.43 magnitude (). In December 2014, a study by an international collaboration of astronomers found a period of 13.33 hours with an amplitude of 0.34 magnitude (). The study selected Lujiaxi because it is a suspected "Barbarian" asteroid with a potentially slow rotation period.
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In October 2006, two rotational lightcurves for Magnitka were obtained from photometric observations by Petr Pravec at Ondřejov Observatory and by John Menke at his Menke Observatory, respectively. Lightcurve analysis gave a concurring rotation period of 6.11 hours with a brightness variation of 0.80 and 0.86 magnitude (), respectively, indicating a non-spheroidal shape for Magnitka. In March 2016, Pierre Antonini obtained a tentative lightcurve, which gave a period of 6.24 hours and an amplitude of 0.85 ().
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This star has a stellar classification of A5 IV, matching an A-type subgiant star. The variable nature of this star was discovered in 1970 at Kitt Peak Observatory. It is a monoperiodic Delta Scuti variable with a cycle period of and an amplitude of 0.060 in visual magnitude; ranging from a peak magnitude of 6.44 down to 6.51. AZ Canis Minoris is nearly a billion years old with a projected rotational velocity of 44 km/s.
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In February 1989, a first rotational lightcurve of Mentha was obtained from photometric observations by Polish astronomer Wiesław Wiśniewski. Lightcurve analysis gave a well-defined rotation period of 85 hours with a brightness variation of 0.87 magnitude (). In February 2013, a similar period of 82.870 hours with an amplitude of 0.65 magnitude was measured by astronomers at the Palomar Transient Factory in California (). A high brightness amplitude is typically indicative for an elongated rather than spherical shape.
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Two rotational lightcurve of Cottrell were obtained from photometric observations by astronomers at the Palomar Transient Factory in California. Analysis gave an identical rotation period of 4.499 hours for both lightcurves and a brightness variation of 0.42 and 0.44 magnitude, respectively (). In February 2012, photometry at the Etscorn Campus Observatory (), New Mexico, gave a well-defined period of 4.4994 hours with an amplitude of 0.77 magnitude, which indicates that the body has a non- spheroidal shape ().
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In October and November 2003, two rotational lightcurves of Rusthawelia were obtained from photometric observations by John Menke at his observatory in Barnesville, Maryland, and by a group of American astronomers. Lightcurve analysis gave a well-defined rotation period of 10.80 and 10.98 hours and a brightness variation of 0.31 and 0.26 magnitude, respectively (). A third, concurring period of 11.013 hours with an amplitude of 0.26 magnitude was obtained by French amateur astronomer René Roy in February 2005 ().
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Two rotational lightcurves of Johnmckay were obtained for this asteroid from photometric observations by U.S. astronomer Brian D. Warner at the Palmer Divide Station (PDO), Colorado. In August 2010, the first lightcurve gave a long rotation period of hours with a brightness variation of 1.0 in magnitude (). The second lightcurve from June 2015, gave a similar period of with an amplitude of 0.66 in magnitude (). This makes Johnmckay one of the Top 100+ slowest rotators known to exist.
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The star has a stellar classification of B8 III, matching a B-type giant. Absorption lines in the spectrum are displaying central quasi-emission peaks, indicating this is a Be shell star with a circumstellar disk of heated gas that is being seen edge- on. ν Puppis is a candidate variable star showing an amplitude of 0.0117 magnitude with a frequency of 0.15292 per day. It is spinning rapidly with a projected rotational velocity of 225 km/s.
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Between 1998 and 2005, a survey of members of the Koronis family by seven different observatories obtained a large number of rotational lightcurves from . For Vltava, the survey gave an ambiguous rotation period of 34.0 hours with a brightness variation of 0.21 in magnitude (). In 2014, photometric observations at the Palomar Transient Factory in California rendered a lightcurve with an alternative solution of hours, or about half the period previously found, with an amplitude of 0.19 magnitude ().
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In December 2017. a rotational lightcurve of Fragaria was obtained from photometric observations by American photometrist Tom Polakis at the Command Module Observatory in Arizona. Lightcurve analysis gave a rotation period of hours with a brightness variation of magnitude (). Since the 1990s, the best period determinations was mady by French and Italian astronomers at ESO's La Silla Observatory using the ESO 1-metre telescope which gave 10.88 hours (or twice the period solution) and an amplitude of 0.12 magnitude ().
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Jean Meeus suspected that was a Mars Trojan, and this was confirmed by Reiner Stoss's analysis of two sets of observations dating from 1998 on the MPC database. It was confirmed to be a Mars Trojan numerically in 2012. Recent calculations confirm that it is a stable Mars Trojan asteroid with a libration period of 1310 years and an amplitude of 14°. These values as well as its short-term orbital evolution are similar to those of 5261 Eureka.
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LP Andromedae (often abbreviated to LP And) is a carbon star in the constellation Andromeda. It is also a Mira variable whose mean apparent visual magnitude is 15.12 and has pulsations with an amplitude of 1.50 magnitudes and a period of 614 days. In 1974 LP Andromedae, known then as IRC+40540, was identified as a carbon star and also shown to be variable. It had previously been suspected of variability during the 2 Micron All Sky Survey (2MASS).
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In September 2005, a rotational lightcurve of Astrid was obtained from photometric observations by French amateur astronomer René Roy. Lightcurve analysis gave a rotation period of 10.228 hours with a brightness variation of 0.29 magnitude (). In October 2010, additional lightcurves were obtained at the Palomar Transient Factory in California, as well as by astronomers Eric Barbotin and Raoul Behrend, which gave a concurring period of 10.2 and 10.229 hours with an amplitude of 0.10 and 0.13 magnitude, respectively ().
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At that distance, the brightness of the star is diminished by 0.21 in magnitude from extinction caused by interstellar gas and dust. This is a red giant star with a stellar classification of M0 III. It is a semi-regular variable with periods of 32 and 275 days; the brightness of the star changes by an amplitude of 0.14 in magnitude during those intervals. The measured angular diameter of this star, after correction for limb darkening, is .
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The star is moving further from the Earth with a heliocentric radial velocity of −27 km/s. It has a relatively high proper motion, traversing the celestial sphere at the rate of per year. The stellar classification of 23 And is F0 IV, matching an F-type subgiant star that is in the process of evolving into a red giant. It displays a slight microvariability with a frequency of 0.85784 d−1 and an amplitude of 0.0062 magnitude.
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The Morning Glory cloud is a rare meteorological phenomenon consisting of a low-level atmospheric solitary wave and associated cloud, occasionally observed in different locations around the world. The wave often occurs as an amplitude-ordered series of waves forming bands of roll clouds. The southern part of the Gulf of Carpentaria in Northern Australia is the only known location where it can be predicted and observed regularly due to the configuration of land and sea in the area.
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In March 1988, Polish astronomer Wiesław Z. Wiśniewski obtained a lightcurve of Simonida that gave a rotation period of 5.3 hours with a brightness variation of 0.26 magnitude (). In January 2004, astronomer A. Kryszczynska at Poznań Observatory measured a period of 5.2885 hours with an amplitude of 0.50 magnitude (). In January 2008, photometric observations by astronomers Martine Castets, Bernard Trégon, Arnaud Leroy and Raoul Behrend gave a rotation period of 5.16 hours with a brightness variation of 0.21 ().
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In September 2000, American astronomer Brian Warner obtained two rotational lightcurves, giving a rotation period of 5.867 and 5.87 hours with a brightness variation of 0.50 and 0.55 magnitude, respectively (). In February 2006, photometric observations by French amateur astronomer Laurent Bernasconi gave a concurring period of 5.873 hours with an amplitude of 0.55 magnitude (). This well- defined period was further confirmed by a modeled light-curve using data from the Lowell Photometric Database, giving a period of 5.87016 hours ().
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The single listener model in OpenAL is tailored to a single human user and is not fit for artificial intelligence or robotic simulations or multiple human participants as in collaborative musical performances. In these cases a multiple listener model is required. OpenAL also fails to take into account sound propagation delays (the speed of sound is used for the Doppler effect only). The distance to a sound source only translates into an amplitude effect (attenuation) and not a delay.
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The first valid rotational lightcurve of Strackea with a period of 4.05 hours and a brightness variation of 0.17 magnitude was obtained by French amateur astronomer Laurent Bernasconi in February 2006 (). Since then, several well-defined lightcurves with a period between 4.044 and 4.052 hours and an amplitude of 0.15 to 0.25 magnitude were obtained by astronomers Brian Warner, Richard Schmidt, as well as by the group of astronomers Pierre Antonini, Raoul Behrend, Roberto Crippa and Federico Manzini ().
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In August 1995, a rotational lightcurve of Palamedes was obtained from photometric observations by Stefano Mottola and Hans-Josef Schober using the now decommissioned Bochum 0.61-metre Telescope at ESO's La Silla Observatory in Chile. Lightcurve analysis gave a rotation period of hours and a brightness variation of 0.05 magnitude (). A more refined period of hours with an amplitude of 0.27 magnitude was obtained by Robert Stephens at the Goat Mountain Astronomical Research Station in October 2009 ().
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Both detectors are expected to be sensitive to periodic spacetime strains of h ~ , given as an amplitude spectral density. The INFN Genoa detector is a resonant antenna consisting of two coupled spherical superconducting harmonic oscillators a few centimeters in diameter. The oscillators are designed to have (when uncoupled) almost equal resonant frequencies. The system is currently expected to have a sensitivity to periodic spacetime strains of h ~ , with an expectation to reach a sensitivity of h ~ .
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In the Tholen classification, Anagolay is a silicaceous S-type asteroid. Based on two rotational lightcurves obtained in the 1980s, Anagolay has a rotation period of 9.012 hours and a brightness variation of 0.20 and 0.21 in magnitude, respectively (). A third lightcurve, also from the 1980s, gave an alternative period of hours with an amplitude of 0.14 (). The body's albedo lies between 0.18 and 0.34, with the Collaborative Asteroid Lightcurve Link (CALL) deriving an intermediate albedo of 0.26.
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This is an aging red giant star on the asymptotic giant branch with a stellar classification of M3 III. It is a semiregular variable with an amplitude of 0.14 in the B-band and pulsation periods of 22.9 and 24.0 days. Having exhausted the hydrogen at its core, the star has expanded to 86 times the Sun's radius. It is radiating 1,202 times the Sun's luminosity from its swollen photosphere at an effective temperature of 3,535 K.
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Its variability was discovered by accident in 1981, when the star was used as a comparison star for the eclipsing binary AG Phoenicis. Photometric and spectroscopic data have allowed the detection of at least 13 modes of radial and non-radial pulsations, the strongest one having a period of 0.174 days and an amplitude of 11.1 milli-magnitudes. Observations in different epochs show evidence that the pulsations modes vary in amplitude, which is common among Delta Scuti variables.
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In July 2005, a rotational lightcurve of Wright was obtained by astronomers Reiner Stoss, Jaime Nomen, Salvador Sánchez and Raoul Behrend at the Mallorca Observatory, Spain. Lightcurve analysis gave a well-defined rotation period of hours with a brightness variation of 0.61 magnitude (). In July 2014, another, concurring lightcurve with a period of hours and an amplitude of 0.53 was obtained by Robert Stephens at the Trojan Station of the Center for Solar System Studies () in Landers, southern California.
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Plate detector circuit with cathode bias. Cathode bias RC time constant three times period of lowest carrier frequency. CL is typically around 250 pF. In electronics, a plate detector (anode bend detector, grid bias detector) is a vacuum tube circuit in which an amplifying tube having a control grid is operated in a non-linear region of its grid voltage versus plate current transfer characteristic, usually near plate current cutoff, in order to demodulate an amplitude modulated carrier signal.
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In May 2005, the first rotational lightcurve was obtained for this asteroid from photometric observations made by French amateur astronomer Laurent Bernasconi. It gave a rotation period of hours with a brightness variation of 0.44 magnitude (). Between May 2010 and December 2014, American astronomer Brian D. Warner obtained another 3 well-defined lightcurves at the U.S. Palmer Divide Station, Colorado. They gave a slightly longer period of 5.193–5.203 hours with an amplitude of 0.28 to 0.42 magnitude ().
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In May 2014, a photometric lightcurve analysis by American astronomer Robert Stephens at the Center for Solar System Studies (), California, gave a rotation period of hours with a brightness variation of 0.26 in magnitude (). Alternative measurements also made in 2014, include an observation by astronomer René Roy, which rendered a period of hours with an amplitude of 0.31 in magnitude (), and an analysis at the Burleith Observatory (), with a period of hours, or 49% of the first period ().
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Italian astronomer Stefano Mottola obtained two concurring rotational lightcurves from photometric observations. In June 1994, together with astronomer Anders Erikson, he constructed a lightcurve from observations made with the 0.9-meter Dutch telescope at La Silla, showing a rotation period of hours and a brightness variation of magnitude (). In September 2009, he used the 1.2-meter reflector at Calar Alto Observatory, Spain, and measured a refined period of hours with an amplitude of in magnitude (), confirming his previous result.
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All told, the booster burns for 0.5 second and the driving engine for another 2.0 seconds. The missile's uncooled lead sulfide passive infra-red seeker head detects infrared radiation at below 2.8 μm in wavelength. It has a 1.9 degree field of view and can track at 9 degrees per second. The seeker head tracks the target with an amplitude-modulated spinning reticle (spin-scan or AM tracking), which attempts to keep the seeker constantly pointed towards the target.
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R85 (or RMC 85, after the Radcliffe Observatory Magellanic Clouds catalog) is a candidate luminous blue variable located in the LH-41 OB association in the Large Magellanic Cloud. R85 has been shown to vary erratically in brightness with an amplitude of about 0.3 magnitudes. It shows variations on several timescales, sometimes with a distinct 400 day period. It has also shown temperature changes associated with brightness changes over several years, a characteristic of Luminous Blue Variables.
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In March 2009, a rotational lightcurve of Timhunter was obtained from photometric observations by astronomer Petr Pravec at the Ondřejov Observatory in the Czech Republic. Lightcurve analysis gave a well-defined rotation period of 14.55 hours with a brightness variation of 0.29 magnitude (). One month later, another lightcurve was obtained by French amateur astronomers David Romeuf, Maurice Audejean and René Roy, which gave an alternative period solution of 7.1074 hours with an amplitude of 0.32 magnitude ().
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In July 2005, a rotational lightcurve of Tergeste was obtained by several photometrists including Laurent Bernasconi, Reiner Stoss, Petra Korlević and Raoul Behrend. The light-curve gave a rotation period of hours with a brightness variation of 0.23 in magnitude (), superseding a period of hours from the 1980s (). In January 2013, another lightcurve was obtained during a photometric survey by predominantly Polish and Japanese observatories. It gave a similar period of hours with an amplitude of 0.30 magnitude ().
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In September 2002, a rotational lightcurve of Vinifera was obtained from photometric observations by Maurice Clark at the Goodsell Observatory in Minnesota. Lightcurve analysis gave a well-defined rotation period of hours with a brightness variation of magnitude (). Other observation by Jean-Gabriel Bosch, Jacques Michelet and René Roy (2002), Brian Uzpen and Steven Kipp (2002), as well as René Roy and Eric Barbotin (2019), gave nearly identical periods of , and hours with an amplitude of , and magnitude, respectively ().
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In February 2016, a rotational lightcurve of Athanasia was obtained from photometric observations by Frederick Pilcher at the Organ Mesa Observatory in New Mexico, United States. Analysis gave a classically shaped, well-defined bimodal lightcurve with a rotation period of hours and a very high brightness variation of magnitude, indicative of an highly elongated shape (). In May 2013, Pilcher already observed the object and reported a ambiguous period of or hours with an amplitude of magnitude ().
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It was identified as Mars trojan by H. Scholl, F. Marzari and P. Tricarico in 2005 and its dynamical half-lifetime was found to be of the order of the age of the Solar System. Recent calculations confirm that it is indeed a stable Mars trojan with a libration period of 1365 yr and an amplitude of 11°. These values as well as its short-term orbital evolution are very similar to those of 5261 Eureka.
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In March 2015, three rotational lightcurves of Daléra were independently obtained by Italian astronomers Maurizio Scardella (), Fabio Salvaggio (), and Giovanni Casalnuovo () after being reported as a light-curve photometry opportunity at minorplanet.info (CALL). They gave a rotation period of 3.880 and 3.881 hours with a brightness variation of 0.18 and 0.14 magnitude, respectively (). Previously, photometric observations at the Palomar Transient Factory in September 2013, gave a longer period of 4.2227 hours and an amplitude of 0.14 magnitude ().
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Other F-type stars include Procyon's primary star, the brightest star in the constellation Canis Minor. The supergiant pulsates, showing small variations in its brightness and spectral lines. The pulsations have been given periods of 67 and 123 days, with an amplitude of about 0.05 magnitudes. The profiles of many spectral lines show variations that would be expected from a pulsating spergiant, but it isn't clear if they have the same period as the brightness variations.
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The signal of the PSD is amplified by a preamplifier. An amplitude control (4) measures the amplitude A of this signal and a feedback loop compares it with a setpoint and determines the amplification (dissipation Γ) of the excitation signal (6) for the cantilever which is fed to a shaking piezo. To measure the current resonance frequency, a phase-locked loop (PLL) (5) is used. Its voltage- controlled oscillator (VCO) produces the excitation signal (6) for the cantilever.
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To generate interference fringes, light from the source has to be divided into two waves which have then to be re-combined. Traditionally, interferometers have been classified as either amplitude-division or wavefront-division systems. In an amplitude-division system, a beam splitter is used to divide the light into two beams travelling in different directions, which are then superimposed to produce the interference pattern. The Michelson interferometer and the Mach–Zehnder interferometer are examples of amplitude-division systems.
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A phase modulating EOM can also be used as an amplitude modulator by using a Mach–Zehnder interferometer. A beam splitter divides the laser light into two paths, one of which has a phase modulator as described above. The beams are then recombined. Changing the electric field on the phase modulating path will then determine whether the two beams interfere constructively or destructively at the output, and thereby control the amplitude or intensity of the exiting light.
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Several rotational lightcurves of ' have been obtained from photometric observations. In June 2006, Lawrence Molnar at Calvin University determined a rotation period of hours with a brightness variation of 0.37 magnitude, using the Calvin-Rehoboth Robotic Observatory in New Mexico.(). In September 2008 observations at the Roque de los Muchachos Observatory gave a period of 18.854 hours with an amplitude of 0.22 magnitude (), while astronomers at the Palomar Transient Factory obtained a period of 18.917 hours in the R-band in October 2010 ().
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In May 2015, a rotational lightcurve of Aralia was obtained from photometric observations by Julian Oey, Hasen Williams and Roger Groom at the Blue Mountains Observatory and Darling Range Observatory (DRO). Lightcurve analysis gave a rotation period of hours with a brightness variation of magnitude (). Alternative observations by Robert Stephens at the Santana Observatory in 2001 and Michael S. Alkema at the Elephant Head Observatory in 2012, gave a similar period determination of and hours, with an amplitude of and , respectively ().
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In August 2010, a rotational lightcurve of Chlosinde was obtained from photometric observations by Robert Stephens at the Santana Observatory and Goat Mountain Astronomical Research Station in California. Lightcurve analysis gave a rotation period of hours with a low brightness variation of magnitude, indicative of a rather spherical shape (). However the result is ambiguous with an alternative period solution of hours. In September 2010, Larry Owings determined at period of hours with an amplitude of magnitude at the Barnes Ridge Observatory in California ().
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This is an evolved K-type giant star with a stellar classification of K5 III. It is a suspected variable with an amplitude of 0.03 magnitude. The measured angular diameter of the star after correcting for limb darkening is , which, at the estimated distance of this star, yields a physical size of about 46 times the radius of the Sun. The star is radiating around 560 times the solar luminosity from its outer atmosphere at an effective temperature of 3,940 K.
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They gave a revised rotation period for the primary of 3.7814 to 3.7824 hours with a brightness variation between 0.10 and 0.20 magnitude (). These observations also confirmed that Johnson is a binary system, giving a concurring orbital period of 21.78 to 21.797 hours for the satellite. For an asteroid of its size, Johnson has a somewhat fast spin rate, but still significantly above those of fast rotators. CALL adopts a rotation period of 3.7824 hours with an amplitude of 0.20 magnitude.
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In September 2013, a first rotational lightcurve of Idaios was obtained from photometric observations in the R-band by astronomers at the Palomar Transient Factory in California. Lightcurve analysis gave a rotation period of 15.733 hours with a brightness amplitude of 0.22 magnitude (). Between 2013 and 2017, three additional period determinations were made by Robert Stephens at the Center for Solar System Studies, with the best-rated lightcurve from 2014 showing a more refined period hours and an amplitude of 0.22 magnitude ().
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In 2012 and 2013, three rotational lightcurves of Glaukos in the R- and S-band were obtained by astronomers at the Palomar Transient Factory in California. Lightcurve analysis gave a rotation period of 5.979, 5.980 and 5.989 hours with an amplitude between 0.27 and 0.37 magnitude (). In October 2013, photometric observations by American astronomer Robert Stephens at the Center for Solar System Studies gave the so-far best rated lightcurve, with a period of hours and a brightness variation of 0.42 magnitude ().
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In March 1992, the first reliable rotational light curve of Golia was obtained by Italian astronomer Mario Di Martino using the ESO 1-metre telescope at La Silla in northern Chile. Analysis gave a well-defined rotation period of 4.097 hours with a change in brightness of 0.35 magnitude (). Another light curve was obtained from photometric observations in the R-band at the Palomar Transient Factory in October 2011, giving a period of 4.0910 hours and an amplitude of 0.24 magnitude ().
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A rotational lightcurve of Disa was obtained by American astronomer Brian D. Warner at his Palmer Divide Observatory in March 2006, and by French amateur astronomer Pierre Antonini in February 2011, respectively. Analysis of both lightcurves gave a well-defined rotation period of 7.08 hours with a brightness variation of 0.26 and 0.27 magnitude (). In September 2013, photometric observations in the R-band at the Palomar Transient Factory gave a concurring lightcurve of 7.082 hours and an amplitude of 0.24 magnitude ().
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In February 1994, a rotational lightcurve of Dares was obtained over five nights of observation by Stefano Mottola and Anders Erikson using the ESO 1-metre telescope at La Silla Observatory in Chile. Lightcurve analysis showed a well-defined rotation period of hours with a brightness variation of 0.24 magnitude (). In October 2013, photometric observations in the R-band by astronomers at the Palomar Transient Factory in California gave a concurring period of 18.967 hours with an amplitude of 0.23 magnitude ().
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Several rotational lightcurves of Espinette have been obtained. In April 2011, photometric observations by American astronomer Brian A. Skiff rendered a well-defined rotation period of hours with a brightness variation of 0.25 magnitude (). In August 2015, another observation by Robert Stephens at the Center for Solar System Studies (), California, gave an identical period of with an amplitude of 0.44 magnitude (). Previous observations by Polish astronomer Wiesław Z. Wiśniewski in 1987, and by Italian Federico Manzini in 2005, rendered similar results ().
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In November 2007, American astronomer James W. Brinsfield obtained the first ever lightcurve of Aletta with period of 19.7 hours and a brightness variation of 0.32 magnitude at Via Capote Observatory (). Two more lightcurves were obtained by Australian astronomer Julian Oey at Leura/Kingsgrove Observatory in March 2010, and by the Survey conducted at the Palomar Transient Factory, California, in October 2012. Lightcurve analysis gave a concurring rotation period of 20.39 and 20.3903 hours with an amplitude of 0.28 and 0.27 magnitude, respectively ().
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In February 2006, a rotational lightcurve of Osita was obtained from photometric observation by French amateur astronomer René Roy, giving a well-defined rotation period of 3.81880 hours with a brightness variation of 0.48 magnitude (). Photometric observations in the R-band at the Palomar Transient Factory in October 2011, gave a concurring period of 3.8186 hours and an amplitude of 0.59 magnitude (). A third period of 3.81880 hours was derived from a large international data-mining collaboration in February 2016 ().
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In March 2013, two rotational lightcurves of Lexell were obtained from photometric observations by Gary Haagen at Stonegate Observatory, Massachusetts, and by a group of astronomers at the Oakley Southern Sky Observatory (), Australia. Lightcurve analysis gave a well-defined rotation period of 5.441 and 5.4429 hours with a brightness variation of 0.45 and 0.42 magnitude, respectively (). In February 2013, observations made by French amateur astronomer Pierre Antonini gave a concurring period of 5.44 hours with an amplitude of 0.51 magnitude ().
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In November 2007, the first rotational lightcurve of Ruppina was obtained at Whitin Observatory in Massachusetts, United States. Lightcurve analysis gave a well-defined rotation period of 5.880 hours with a brightness variation of 0.35 magnitude (). During the 2014-apparition of Ruppina, an identical period was obtained again at Whitin Observatory (), while photometric observations in the R-band at the Palomar Transient Factory in California, gave a period of 5.890 and 5.9046 hours with an amplitude of 0.27 and 0.28, respectively ().
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This is a metallic-line star with a stellar classification of Fm δ Del, where the suffix notation indicating it is a δ Delphini star. It is a Delta Scuti variable, with a period of and an amplitude of 0.03 magnitude. The star has 4.3 times the girth of the Sun and is spinning with a projected rotational velocity of 45 km/s. It is radiating 34 times the luminosity of the Sun from its photosphere at an effective temperature of 6,704 K.
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They have reached approximately equal levels of carbon and oxygen in their atmospheres, which causes dramatic changes to the atmospheric chemistry which are visible in the spectrum. As an S star, its spectrum is classified as S5,1, with S5 approximately equivalent to the temperature of an M5 giant and the 1 indicating that the ZrO bands are relatively weak. BQ Octantis is a variable star. An amplitude of 0.05 magnitudes about an apparent magnitude of 6.82 has been derived from Hipparcos satellite photometry.
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A first rotational lightcurve of Augeias was obtained from by Linda French and Lawrence Wasserman in April 2014. Lightcurve analysis gave a tentative rotation period of hours with a brightness amplitude of 0.15 magnitude (). In August 2015, photometric observations by the Kepler space telescope during its K2 mission determined a refined period of hours with a brightness variation of 0.15 magnitude (). One week later, a second, lower-rated lightcurve by Kepler gave a concurring period of hours with an amplitude of 0.16 ().
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Between 2005 and 2014, a large number of rotational lightcurves of Pólit were obtained from photometric observations by American astronomer Maurice Clark at the Preston Gott and McDonald Observatories. Lightcurve analysis gave a rotation period of 7.5080 to 7.5085 hours with a brightness variation between 0.40 and 0.50 magnitude (). Clark also derived a spin axis of (2.1°, 47.5°) in ecliptic coordinates (λ, β) (). In addition, astronomer Raymond Poncy measured a period of 7.520 hours with an amplitude of 0.30 magnitude ().
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In December 2005, American amateur astronomer Donald P. Pray obtained a rotational lightcurve at Carbuncle Hill Observatory in collaboration with other astronomers. Light-curve analysis gave a well-defined rotation period of 5.3202 hours with a brightness variation of 0.47 magnitude (). Previous photometric observations were made by Kryszczyńska et al. in July 2004, that gave an identical period with an amplitude of 0.40 magnitude (), and by Claes-Ingvar Lagerkvist, who derived a period of 5.33 hours (Δ0.5 mag) already in the 1970s ().
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Two rotational lightcurve of Vladimir were obtained by Serbian astronomer Vladimir Benishek at the Belgrade Observatory in April 2008, and August 2015. Analysis of the bimodal lightcurve gave a rotation period of 12.57 and 12.582 hours with a relatively low brightness variation of 0.14 and 0.24 magnitude, respectively (). In December 2010, and January 2012, photometric observations in the R-band at the Palomar Transient Factory in California gave a period of 12.574 and 12.557 hours with an amplitude of 0.23 and 0.22, respectively ().
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Two rotational lightcurves of Porzia were obtained by Vladimir Benishek at Belgrade Observatory shortly before its opposition in November 2009, and by French amateur astronomer René Roy in December 2012. Lightcurve analysis gave a well defined rotation period of 4.6584 and 4.6601 hours with a brightness variation of 0.15 and 0.19 magnitude, respectively (). The results supersede photometric observations taken by Polish astronomer Wiesław Wiśniewski in January 1990, which rendered a lightcurve with a period hours and an amplitude of 0.23 magnitude ().
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In September 1984, a rotational lightcurve of Granada was obtained from photometric observations by astronomer Richard Binzel. Lightcurve analysis gave a rotation period of 31 hours with a brightness variation of 0.28 magnitude (). In October 2010, photometric observations in the R-band by astronomers at the Palomar Transient Factory gave a period of 72.852 hours and an amplitude of 0.24 (). While not being a slow rotator, Granadas period is significantly longer than the typical 2 to 20 hours measures for most asteroids.
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In June 2016, a rotational lightcurve of Stentor was obtained from photometric observations by Brian Warner at the Center for Solar System Studies (CS3) in California. Lightcurve analysis gave a rotation period of hours with a brightness amplitude of 0.10 magnitude (). An alternative period solution (1:1.5 alias of 24.88 was also obtained. Stentor was previously observed at CS3 by Daniel Coley and Robert Stephens in February 2013, gave an alternative period solution of hours with an amplitude of 0.09 magnitude.
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In January 2006, a rotational lightcurve of Yukitsuna was obtained from photometric observations by Federico Manzini at the Sozzago Astronomical Station in Italy. Lightcurve analysis gave a rotation period of 19.2 hours with a brightness variation of 0.8 magnitude (). In September 2008, a more refined period of 19.04 hours and an amplitude of 0.80 magnitude was measured at the Oakley Southern Sky Observatory and Oakley Observatory (). The high brightness variation of 0.8 magnitude is indicative for an elongated, non-spherical shape.
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In March 1984, the first but poorly rated rotational lightcurve of Summa was obtained from photometric observations by American astronomer Richard Binzel. It gave a rotation period of 9.66 hours with a brightness amplitude of 0.14 magnitude (). In August 2012, a refined yet ambiguous lightcurve with a period of 6.855 hours and an amplitude of 0.13 was obtained by Larry E. Owings at the Barnes Ridge Observatory in California (). Lightcurve analysis also considered that Summa might be a binary system.
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In October 1999, two rotational lightcurves of Tone were obtained from photometric observations by American astronomer Brian Warner at his Palmer Divide Observatory () in Colorado. Lightcurve analysis gave two divergent rotation periods of 7.40 and 11.82 hours with a brightness variation of 0.06 and 0.12 magnitude, respectively (). Observation by Italian astronomers Roberto Crippa and Federico Manzini in October 2005, gave another tentative period of 12.9 hours and an amplitude of 0.07 magnitude (). The LCDB currently adopts a period of 7.40 hours.
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The SFE technology was developed at the University of Washington for the purpose of providing high-quality laser-based imaging within an ultrathin and flexible endoscope. It is believed that the concept of moving an optical fiber to produce 2D images with confocal sectioning and laser illumination was first proposed for endoscopic applications by Giniunas et al., in 1993. A major advancement of the SFE is rapid scanning and generation of high-quality images using an amplitude-modulated resonating fiber.
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In May 2003, a rotational lightcurve of Columbia was obtained by French amateur astronomer René Roy. It gave a rotation period of 5.93 hours with a brightness variation of 0.16 magnitude (). In February 2007, photometric observations by his college Pierre Antonini gave a well defined period of 5.9320 hours and an amplitude of 0.42 (). In 2016, a modeled lightcurve was derived from various photometric database sources, giving a concurring period of 5.93183 hours and a spin axis of (52.0°, 43.0°) in ecliptic coordinates.
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Stellar occultation events indicate that Gǃkúnǁʼhòmdímà has an effective (equivalent-sphere) diameter of 600–670 km, but is not spherical. Due to complications from its non-spherical shape, the rotational period cannot be definitely determined from current light-curve data, which has an amplitude of Δm = 0.03 ± 0.01 mag, but the simplest solution is 11.05 hours. It is almost certainly between that and 41 hours. The system mass is , about 2% that of Earth's moon and a bit more than Saturn's moon Enceladus.
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This is an evolved red giant star with a stellar classification of M2.5 IIIb. It is a semiregular variable that ranges between magnitudes 5.11 and 5.17. Hipparcos mission photometry gives an amplitude variation of 0.0148 in magnitude with a frequency of 11.4 cycles per day. In terms of its right ascension coordinates, φ Pegasi is located very near the line of the vernal equinox and will cross over around the year 3030, due to the precession of the Earth's axis.
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It is drifting further away with a heliocentric radial velocity of +12.5 km/s. The primary component is an evolved giant star with a stellar classification of G8 III. It is a periodic variable star, showing a change in brightness with an amplitude of 0.004 magnitude at the rate of 7.50983 times per day. With the supply of hydrogen at its core exhausted, the star has cooled and expanded until now it has 10 times the radius of the Sun.
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A large number of rotational lightcurves of Tama were obtained from photometric observations since it has been identified as a binary asteroid (see below). Lightcurve analysis gave a rotation period between 16.4 and 16.464 hours with a brightness variation between 0.08 and 0.41 magnitude (), superseding a period of 4 hours from a fragmentary lightcurve obtained in the 1990s (). Tama appears to be somewhat elongated in shape. LCDB's consolidated result gives a period of 16.44 hours and an amplitude of 0.41 magnitude ().
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In January 2004, the first rotational lightcurves of Skuld were obtained by Henk de Groot and by a group of Polish and French astronomers. Lightcurve analysis gave a rotation period of 4.73 and 4.8079 hours with a brightness variation of 0.46 and 0.40 magnitude, respectively (). In 2009 and 2011, astronomers Robert Buchheim and Larry Robinson obtained two well-defined lightcurves from photometric observations. They gave a refined period of 4.810 and 4.807 hours with an amplitude of 0.50 and 0.26 magnitude, respectively ().
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The brightness variation is maximum in the v band, with an amplitude of 0.13 magnitudes. The light curve in this band is symmetrical and has two distinct minima separated by half a rotation period, while the two maxima are igual. In other bands the variability is smaller or even absent, and doesn't show a regular pattern like in v. The star is similar in many aspects to rapidly oscillating Ap stars, but does not display the rapid pulsations typical of these stars.
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Several rotational lightcurves of Quintilla were obtained from photometric observations. Analysis of the best-rated lightcurves by Robert K. Buchheim and Donald Pray (2004), Laurent Bernasconi, Reiner Stoss, Petra Korlević, Maja Hren, Aleksandar Cikota, Ljuban Jerosimic, and Raoul Behrend (2005), as well as Joseph Masiero (2006), gave a well-defined rotation period of (), () and () hours with a brightness variation of (), () and () magnitude, respectively (). In November 2018, Michael and Matthew Fauerbach obtained a period of () hours and an amplitude of () magnitude ().
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The two periods are slightly longer than twice Polakis period solution (). In April 2007, astronomers at the Oakley Observatory , Indiana, obtained a period of hours and an amplitude of magnitude (). In February 2011, French amateur astronomer René Roy determined a period of hours and a brightness variation of magnitude (). A modeled lightcurve by Josef Ďurech and Josef Hanuš, using photometric data including from the Lowell Photometric Database and from the Wide-field Infrared Survey Explorer (WISE) was published in 2018.
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In September 2011, a rotational lightcurve of Melanie was obtained from photometric observations by Robert Stephens at the Santana Observatory in California. Lightcurve analysis gave a well-defined rotation period of hours with a low brightness variation of magnitude (). The first but unsuccessful attempt to measure the objects period was undertaken by Richard Binzel in June 1984. Other observations by French amateur astronomers Laurent Bernasconi (2005) and René Roy (2011) gave a period of () and () hours and an amplitude of and magnitude, respectively ().
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In October 2007, a first rotational lightcurve of Euboea was obtained from photometric observations by astronomers at the Oakley Southern Sky Observatory in Australia. Lightcurve analysis gave a rotation period of 11.41 hours with a brightness variation of 0.50 magnitude (). In April 2010, a similar period of 11.396 hours and an amplitude of 0.46 magnitude was measured by French amateur astronomer Pierre Antonini (). In 2016, two modeled lightcurves were published using photometric data from the Lowell Photometric Database and other sources.
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An amplitude-modulated signal has frequency components both above and below the carrier frequency. If one set of these components is eliminated as well as the residual carrier, only the remaining set is transmitted. This reduces power in the transmission, as roughly of the energy sent by an AM signal is in the carrier, which is not needed to recover the information contained in the signal. It also reduces signal bandwidth, enabling less than one-half the AM signal bandwidth to be used.
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HD 130144 (or EK Boötis) is a semiregular variable star in the northern constellation of Boötes. The variation in luminosity has an amplitude of 0.38 in magnitude with no apparent periodicity. This is an X-ray source, and was possibly the first M-type giant star to have a magnetic field directly detected. It is considered to be a single star, although there is nearby companion at an angular separation of 0.2023″ along a position angle of 82.2° (as of 2010.4812).
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Based upon proper motion variation, this is an astrometric binary system with high likelihood (99.8%). The visible component has a stellar classification of F0 Vn, indicating it is a F-type main-sequence star with "nebulous" lines due to rapid rotation. It is a Delta Scuti variable star with a period of 0.0960 days and an amplitude of 0.020 in magnitude. With 2.4 times the mass of the Sun it is spinning with a high projected rotational velocity of 133 km/s.
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It should achieve perihelion in about two million years, approaching as close as . This is an evolved giant star with a stellar classification of K2 III, having exhausted the supply of hydrogen at its core and moved off the main sequence. It is a suspected variable star, possibly of the micro-variable variety, having an amplitude of less than 0.03 in magnitude. 14 Sagittarii is radiating about 317 times the Sun's luminosity from its photosphere at an effective temperature of around 3,940 K.
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It is a suspected variable star of unknown type, with an I-band brightness ranging from 3.29 down to 3.44 magnitude. Hipparcos photometry revealed a microvariability with a frequency of 0.17017 cycles per day and an amplitude of 0.0080. With the supply of hydrogen exhausted at its core, it has expanded and now has 48 times the Sun's girth. The star is radiating 492 times the luminosity of the Sun from its swollen photosphere at an effective temperature of 3,930 K.
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This is a supergiant star with a stellar classification of K3 Ib, although Houk and Swift (1999) classed it as a normal giant at K3 III. It displays microvariability, undergoing changes in brightness with a frequency of 11.2 times per day and an amplitude of 0.0053 in magnitude. The star is about 30 million years old with nine times the mass of the Sun. It is radiating 10,170 times the Sun's luminosity from its photosphere at an effective temperature of 4,152 K.
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This causes its osculating orbital elements to vary with an amplitude of about 20 km in semi-major axis on a timescale of about 2 Earth years. The close proximity to the orbits of Pallene and Methone suggests that these moons may form a dynamical family. Material blasted off Anthe by micrometeoroid impacts is thought to be the source of the Anthe Ring Arc, a faint partial ring about Saturn co-orbital with the moon first detected in June 2007.
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In September 2009, a first rotational lightcurve of ' was obtained from photometric observations by Linda French at the Cerro Tololo Inter-American Observatory in Chile. Lightcurve analysis gave a rotation period of hours with a brightness variation of 0.10 magnitude (). Since then, follow-up observations by Daniel Coley and Robert Stephens at the Center for Solar System Studies during 2013–2017 gave four more refined lightcurves, with the best-rated one from January 2017 showing a rotation period of hours and an amplitude of 0.26 magnitude ().
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The primary component, Phi Virginis A, has a stellar classification of G2 IV, indicating that it is a G-type subgiant which is evolving away from the main sequence. It is slightly variable with an amplitude of 0m.06. The star has about 1.8 times the mass of the Sun, 4 times the Sun's radius, and shines with 12.6 times the luminosity of the Sun. It is around 1.5 billion years old and is spinning with a projected rotational velocity of 15.5 km/s.
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TSI varies in phase with the solar magnetic activity cycle with an amplitude of about 0.1% around an average value of about 1361.5 W/m2 (the "solar constant"). Variations about the average of up to −0.3% are caused by large sunspot groups and of +0.05% by large faculae and the bright network on a 7-10-day timescale (see TSI variation graphics). Satellite-era TSI variations show small but detectable trends. TSI is higher at solar maximum, even though sunspots are darker (cooler) than the average photosphere.
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In April 210, a rotational lightcurve of Henrika was obtained from six nights of photometric observations by Frederick Pilcher at the Organ Mesa Observatory in New Mexico. Analysis of the classically shaped bimodal lightcurve gave a well-defined rotation period of hours with a brightness variation of magnitude (). During the same apparition, a virtually identical period of hours with an amplitude of magnitude () was determined by Kenda Albers and colleges of the Rose-Hulman Institute of Technology at the Oakley Southern Sky Observatory in Australia.
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Additional observation by the Spanish OBAS group gave a period of hours with an amplitude of magnitude (). In 2016, a modeled lightcurve gave a concurring sidereal period of hours using data from the Uppsala Asteroid Photometric Catalogue, the Palomar Transient Factory survey, and individual observers (such as above), as well as sparse-in-time photometry from the NOFS, the Catalina Sky Survey, and the La Palma surveys . The study also determined two spin axes of (276.0°, 70.0°) and (90.0°, 39.0°) in ecliptic coordinates (λ, β).
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Lightcurve-based 3D-model of Rogeria In October 2010, a rotational lightcurve of Rogeria was obtained from photometric observations by Thomas A. Polakis at the Command Module Observatory in Arizona. Lightcurve analysis gave a rotation period of hours with a brightness variation of magnitude (). A tentative period determination of hours with an amplitude of magnitude was made by French amateur French astronomer René Roy in July 2012 (). Another observation by Petr Pravec and Peter Kušnirák at Ondřejov Observatory in June 2007 gave a period of 8.09 hours ().
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In June 2015, a rotational lightcurve of Anneliese was obtained from photometric observations by Uruguayan astronomer Eduardo Álvarez at the Los Algarrobos Observatory . Lightcurve analysis gave a well-defined rotation period of hours with a brightness variation of magnitude, indicative of a spherical, non- elongated shape (). At the time Anneliese was one of only 17 three-digit numbered asteroids for which no period was published. In May 2015, Julian Oey at the Blue Mountains Observatory , Australia, determined a concurring period of hours with an amplitude of magnitude ().
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A rotational lightcurve of was obtained from photometric observations made by American astronomer Brian Warner at his Palmer Divide Observatory, Colorado, in February 2015. The ambiguous lightcurve rendered a rotation period of hours with a brightness variation of 0.72 magnitude (), while a second solution gave 6.096 hours (or half of the first period) with an amplitude of 0.43. The Collaborative Asteroid Lightcurve Link assumes a standard albedo for stony asteroids of 0.20 and calculates diameter of 225 meters with an absolute magnitude of 20.6.
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In October 2001, a first rotational lightcurve of Gawain was obtained from photometric observations by an international collaboration of astronomers. Lightcurve analysis gave a rotation period of 11.1098 hours with a high brightness variation of 0.69 magnitude (). Additional lightcurves with a period of 11.581 and 11.5 hours and an amplitude of 0.65 and 1.05, respectively, were obtained by astronomers at the Palomar Transient Factory in California in 2011 and 2013 (). A high brightness amplitude typically indicates that the body has a non-spheroidal shape.
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In September 2005, a rotational lightcurve of Hurukawa was obtained from photometric observations by French astronomer Raymond Poncy. It gave a well-defined, slightly longer-than-average rotation period of hours with a brightness variation of 0.47 in magnitude (). The period was confirmed by observations taken at the U.S. Palomar Transient Factory in August 2010, which rendered a period of hours and an amplitude of 0.17 (), superseding a third period of 16 hours from a fragmentary lightcurve obtained by French astronomer René Roy in 2007 ().
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In July 2015, a rotational lightcurve of Cunningham was obtained from photometric observation by American amateur astronomer Robert Stephens at the Center for Solar System Studies in California. It gave a well- defined rotation period of 7.7416 hours with a brightness variation of 0.17 magnitude (). A similar period of 7.7398 hours with an amplitude of 0.16 was previously obtained by French and Italian amateur astronomers Pierre Antonini and Silvano Casulli in July 2008 (). Other lightcurves gave a shorter period of 4.285 and 5.16 hours ().
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Lightcurve-based 3D-model of Annette The first rotational lightcurve of Annette was obtained by American astronomer Brian Warner at his Palmer Divide Observatory, Colorado, in December 2005. It gave a rotation period of 10.457 hours with a brightness variation of 0.92 magnitude (). In November 2006, a second lightcurve by astronomer Robert Buchheim at Altimira Observatory in southern California gave a concurring period of 10.4595 hours and an amplitude of 0.64 magnitude (). He also noted a significantly fainter absolute magnitude of 14.35 than previously reported.
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In August 2000, a rotational lightcurve of Aisleen was obtained from photometric observations made by Glen Malcolm at the Roach Motel Observatory () in California. The analysis gave a well-defined rotation period of 6.68 hours during which the brightness varied by 0.56 in magnitude (). In April 2014, photometric observations by Brian D. Warner gave a period of 6.683 hours with an amplitude of 0.31 magnitude (). A modeled lightcurve from various data sources gave a concurring period of 6.67597 hours and found a pole of (109°,−68°).
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In March 1993, a rotational lightcurve of Bitias was obtained from photometric observations over four consecutive nights by Stefano Mottola using the ESO 1-metre telescope at La Silla Observatory in Chile. Lightcurve analysis gave a rotation period of 11.582 hours with a brightness variation of at least 0.38 magnitude (). In August 2013, a more refined period determination from observations over seven consecutive nights by Robert Stephens at the Center for Solar System Studies gave a well-defined period of hours with an amplitude of 0.32 magnitude ().
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In September 2004, the best rated rotational lightcurve of Cimmeria was obtained from photometric observations by American astronomer Brian Warner at his Palmer Divide Observatory in Colorado. Lightcurve analysis gave a well- define rotation period of 2.820 hours with a brightness amplitude of 0.31 magnitude (). Astronomer Daniel Klinglesmith obtained a similar period of 2.821 hours with an amplitude of 0.29 magnitude. In addition a modeled lightcurve, using photometric data from various sources, gave a period of 2.820723 hours, as well as a spin axis of (63.0°, n.
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In August 2011, a rotational lightcurve of Polydoros was obtained from photometric observations by Linda French at the Cerro Tololo Inter-American Observatory in Chile. Lightcurve analysis, however, gave an incorrect rotation period of hours with a brightness variation of 0.25 magnitude (). Several subsequent observations during 2014–2018 by Daniel Coley and Robert D. Stephens at the Center for Solar System Studies achieved a good period determination, with the best-rated one from November 2015, which gave a period of hours and an amplitude of 0.17 magnitude ().
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In October 2013, a rotational lightcurve of Kotelnikov was obtained from photometric observations in the R-band by astronomers with the Palomar Transient Factory in California. Lightcurve analysis gave a rotation period of 4.752 hours with a brightness variation of 0.26 magnitude (). In March 2015, Swiss and French astronomers René Roy, Raoul Behrend and José De Queiroz measured a period of 4.9078 hours and an amplitude of 0.21 magnitude (). The astronomers noted that Kotelnikov is likely a binary asteroid, yet more observations are required.
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In July 2013, a rotational lightcurve for this asteroid was obtained from photometric observations by Czech astronomer Petr Pravec at the Ondřejov Observatory. The well-defined lightcurve gave a rotation period of hours with a brightness variation of 0.33 in magnitude (). During the same opposition opportunity, two more lightcurves – obtained by Robert Stephens at the Center for Solar System Studies and by Maurice Clark at the Preston Gott Observatory – gave a similar period of and hours, with an amplitude of 0.35 and 0.31 in magnitude, respectively ().
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In March 2013, a rotational lightcurve of Helina was obtained from photometric observations in the R-band by astronomers at the Palomar Transient Factory in California. Lightcurve analysis gave a rotation period of 44.554 hours with a brightness variation of 0.91 magnitude (). In April 2013, European amateur astronomers Matthieu Bachschmidt, Paul Krafft, Olivier Gerteis, Hubert Gully and Luc Arnold measured a period of 44.9 hours with an amplitude of 0.64 magnitude (). While not being a slow rotator, Helina has a longer-than average period.
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At that range, the visual magnitude of the star is diminished by an extinction of due to interstellar dust. It is moving further from the Earth with a heliocentric radial velocity of +19 km/s. This is an aging red giant star with a stellar classification of M2.5 III, which indicates it has exhausted the hydrogen at its core and evolved away from the main sequence. It is a suspected variable star that may vary in brightness with an amplitude of 0.07 in magnitude.
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Photometric observations dating back to 1946 provide a lengthy record of its pattern of pulsation; it undergoes periodic pulsations with a single period of 0.14088143(3) days, or 7.1 cycles per day. During each cycle, the star's magnitude varies with an amplitude of 0.15 and the radial velocity varies by 10 km s−1. The peak brightness occurs 28.8 minutes following the minimum radial velocity. The outer atmosphere's effective temperature of 6,920 K is one of the lowest known for a Delta Scuti variable.
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Stellar models indicate the primary component is similar in physical properties to the Sun, with 110% of the Sun's mass, 96% of the radius, and shining with almost the same luminosity. The overall metallicity of the star—the abundance of elements other than hydrogen and helium—is similar to the Sun. At a relatively youthful estimated age of one billion years, it is rotating with a period of 9.12 days. Based upon Hipparcos data, it displays a mild variability with an amplitude of 0.06 magnitude.
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The two components are nearly identical chemically peculiar stars, having a combined stellar classification of kA7hF0mF0(IV-V). This notation indicates the calcium K line matches an A7 star, the hydrogen lines an F0 star, and the metal lines an F0 star. Each of the stars is a Delta Scuti variable, with the system having a dominant period of 0.1568 days and an amplitude of 0.0700 in magnitude. Delta Delphini forms the prototype of a class of metal-lined δ Scuti subgiant or giant stars.
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The star has an absolute magnitude of −3.77, and is drifting further away with a radial velocity of +9.9 km/s. This object is a massive, aging bright giant with a stellar classification of K3II-IIb. It is a suspected variable star that fluctuates in magnitude by an amplitude of 0.05 in the B-band of the UBV photometric system. With the supply of hydrogen exhausted at its core, it has evolved of the main sequence and cooled and expanded to 156 times the Sun's radius.
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In 2007, a rotational lightcurve of Actor was obtained from photometric observations at the Sierra Nevada Observatory, using its 1.5-meter telescope. Lightcurve analysis gave a rotation period of 7.284 hours with a brightness variation of 0.30 magnitude (). The same group also published a period determination of hours with an amplitude of 0.33 magnitude in 2010. In July and August 2015, observations by the Kepler space telescope during its K2 mission gave another two lightcurves with a concurring period of 7.28 and 7.281 hours, respectively.
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In August 2006, a rotational lightcurve of Sigrid was obtained from photometric observations at the Mount Tarana and Cecil Observatory in NSW, Australia. Lightcurve analysis gave a rotation period of 43.296 hours with a brightness variation of 0.6 magnitude (). In October 2010, Raymond Poncy found a period of 22.68 hours (or half the previous period solution) and an amplitude of 0.38 magnitude (). While not being a slow rotator, the body's period is significantly longer than the typical 2 to 20 hours seen among the majority of asteroids.
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In April 2011, a rotational light-curve was obtained for this asteroid from photometric observations by American astronomer Brian Skiff. The light-curve gave a well- defined rotation period of hours with a brightness variation of 0.68 in magnitude (). Two other light-curves – obtained at the Palomar Transient Factory, California, in February 2014, and by astronomer Maurice Clark at Texas Tech's Preston Gott Observatory in June 2011 – are in agreement with a period of and hours, and an amplitude of 0.46 and 0.65, respectively ().
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In October 2010, a rotational lightcurve of van den Bos was obtained from photometric observations by astronomers Robert Stephens and David Higgins. It gave a rotation period of 740 hours with a brightness variation of 0.80 magnitude (). It is one of the slowest rotating minor planets (see list) and a suspected tumbler, that has a non-principal axis rotation. At the same time, photometric observations at the Shadowbox Observatory gave an alternative, yet ambiguous period of 155 hours with an amplitude of 0.5 magnitude ().
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This object is drifting closer with a radial velocity of −13 km/s. This is an evolved red giant star with a stellar classification of M2 III. It is a variable star of uncertain type, showing a change in brightness with an amplitude of 0.0114 magnitude and a frequency of 0.22675 cycles per day, or 4.41 days/cycle. It has about 67 times the Sun's radius and is radiating 975 times the Sun's luminosity from its photosphere at an effective temperature of 3,936 K.
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When a voltage is applied, the retardation of laser polarization of the light would be changed while a beam passes through an ADP crystal. This variation in polarization results in intensity modulation downstream from the output polarizer. The output polarizer converts the phase shift into an amplitude modulation. Micrometre-scale silicon electro-optic modulatorNature 435, 325–327 (19 May 2005) This device was fabricated a shape of the p-i-n ring resonator on a silicon-on-insulator substrate with a 3-mm-thick buried oxide layer.
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In July 2013, the so-far best-rated rotational lightcurve of Croatia was obtained by astronomers Romain Montaigut, Arnaud Leroy, Raoul Behrend, René Roy, Donn Starkey, Maurice Audejean, Roberto Crippa and Federico Manzini. Lightcurve analysis gave a longer-than average rotation period of 24.821 hours with a brightness variation of 0.25 magnitude (). The result supersedes photometric observations by Brian Warner and by astronomers at the Palomar Transient Factory, which measured a shorter period of 11.7 and 16.385 hours with an amplitude of 0.16 and 0.32, respectively ().
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In May 2011, a rotational lightcurve of Marghanna was obtained from photometric observations by American astronomer Brian Skiff and collaborators using telescopes at the Lowell Observatory in Flagstaff, Arizona. The 2019-revised lightcurve analysis gave a well-defined rotation period of () hours with a small brightness variation of () magnitude, indicative of a rather spherical shape (). Lower rated measurements determined a period of 15.95 hours (Rafa Mohamed, 1995), 24 hours (Raymond Poncy, 2005) and hours (Brian Skiff, 2014) with an amplitude of , and magnitude, respectively ().
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These fields can have both an amplitude, or intensity, and a preferred direction in which they oscillate, or polarization. The polarized signal that CLASS will attempt to measure is incredibly small. It is expected to be only a few parts-per-billion change in the polarization of the already-cold 2.725 K CMB. To measure such a small signal, CLASS will employ focal plane arrays with large numbers of feedhorn-coupled, transition-edge-sensor bolometers cooled to just 0.1 °C above absolute zero by cryogenic helium refrigerators.
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Analysis of Hipparcos photometry shows an amplitude of 0.082 magnitudes and a primary period of 4.76 days. It has not yet been assigned a variable star designation in the General Catalogue of Variable Stars and is still formally listed as a suspected variable. The hydrogen-rich WN stars have been referred to as WNL stars or as WNH stars since they do not necessarily have late nitrogen-sequence spectra. They are systematically more massive and more luminous than stars with similar spectra but lacking nitrogen.
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In the literature, there are two different stellar classifications for this star: A2 Ib and A6 Ib. In either case it is an A-type supergiant star with an estimated age of 30 million years and a mass 8.8 times that of the Sun. It shines with a luminosity 5,798 times the Sun's from an outer atmosphere that has an effective temperature of 6,372 K. As with other stars of its type, ι2 Scorpii varies slightly in brightness, showing an amplitude of 0.05 in magnitude.
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The 'n' suffix indicates "nebulous" absorption lines due to rapid rotation, and it shows a relatively high projected rotational velocity of 109.2 km/s. It is a variable star of unknown type that varies in brightness with an amplitude of 0.05 magnitude. The star is about 570 million years old and it has an estimated mass of 1.47 times the mass of the Sun. On average, it is radiating 25 times the Sun's luminosity from its photosphere at an effective temperature of 7,240 K.
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It is classified as a semiregular variable star, showing a periodicity of 66.8 days with an amplitude of 0.0202 in visual magnitude. Iota Tucanae is an X-ray source with a luminosity of . It has an estimated 2.2 times the mass of the Sun, and, at the age of 1.69 billion years, it has evolved away from the main sequence, expanding to 11 times the Sun's radius. The star radiates 65 times the solar luminosity from its photosphere at an effective temperature of 5,039 K.
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It forms a suspected ellipsoidal variable with a period of 80 days and an amplitude variation of 0.08 in magnitude. The primary component is an aging red giant/bright giant with a stellar classification of M1/M2II/III, currently on the asymptotic giant branch. With the supply of hydrigen at its core exhausted, it has expanded to 160 times the girth of the Sun. It is radiating 3,562 times the luminosity of the Sun from its enlarged photosphere at an effective temperature of 3,562 K.
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Reduced-carrier transmission is an amplitude modulation (AM) transmission in which the carrier signal level is reduced to reduce wasted electrical power. Suppressed-carrier transmission is a special case in which the carrier level is reduced below that required for demodulation by a normal receiver. Reduction of the carrier level permits higher power levels in the sidebands than would be possible with conventional AM transmission. Carrier power must be restored by the receiving station to permit demodulation, usually by means of a beat frequency oscillator (BFO).
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In October 2004, a rotational lightcurve of Newcombia was obtained from photometric observations by American amateur astronomer Walter R. Cooney Jr. in collaboration with John Gross, Dirk Terrell, Vishnu Reddy and Ron Dyvig. Lightcurve analysis gave a well-defined rotation period of hours with a brightness variation of magnitude (). An identical period of hours with an amplitude of magnitude was determined in April 2014, by Daniel Klinglesmith and colleagues at the Etscorn Observatory in New Mexico (). Klinglesmith also published a period of in November 2015 and January 2017 ().
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In February 1984, a rotational lightcurve of Backlunda was obtained from photometric observations by Richard Binzel. Lightcurve analysis gave a rotation period of hours with a brightness variation of magnitude (). In May 2019, an alternative period determination of hours with an amplitude of magnitude was made by Tom Polakis at the Command Module Observatory in Arizona (). Additional, tentative lightcurves gave a period of () by French amateur astronomer Laurent Bernasconi in July 2004, () by Jean-Gabriel Bosch and Axel Martin in March 2007, and () by Bruno Christmann, David Augustin and Raoul Behrend in July 2019 ().
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In January 2007, a rotational lightcurve of Zubaida was obtained from photometric observations by Colin Bembrick at the Mount Tarana Observatory and Greg Crawford at Bagnall Beach Observatory in collaboration with two other Australian observers. Lightcurve analysis gave a well-defined rotation period of hours with a brightness variation of magnitude (). The observers also estimate an axial ratio (a/b) of 1.42 for the asteroid. An alternative observation during January 2007, by David Higgins and Julian Oey at Hunters Hill and Leura observatories, respectively, gave a concurring period hours with an amplitude of magnitude ().
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In November 2006, a rotational lightcurve of Parysatis was obtained from photometric observations by Serbian astronomer Vladimir Benishek at Belgrade Observatory. Lightcurve analysis gave a well-defined rotation period of hours with a brightness variation of magnitude (). The result supersedes other period determinations of () by Marcos Florczak in 1996, () by Laurent Bernasconi in 2003, and () by Michael Fleenor in 2006, and by Andy Monson in 2011 (). In April 2017, another lightcurve with a well-defined period of hours and an amplitude of magnitude was obtained by the Spanish group of asteroid observers, OBAS ().
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In June 2006, a rotational lightcurve of Erda was obtained from photometric observations by David Higgins at Hunters Hill Observatory , Australia, and by Rui Gonçalves at Linhaceira Observatory in Portugal. Lightcurve analysis gave a well-defined rotation period of hours with a brightness variation of magnitude, significantly higher than previous observations had measured (). The observers also found no indication of a previously speculated companion. The result supersedes observations from July 2001, when both Robert Stephens and Laurent Bernasconi determined a period of and hours with an amplitude of and magnitude, respectively.
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Lightcurve based 3D-model of Picka In April 2007, a rotational lightcurve of Picka was obtained from photometric observations by French amateur astronomer Pierre Antonini. Lightcurve analysis gave a well-defined rotation period of hours with a high brightness variation of magnitude, indicative of an elongated shape (). Alternative and lower-rated photometric observations were made by Jean-Gabriel Bosch in February 2006, and again by Pierre Antonini in November 2010, which gave a period of and hours with an amplitude of and magnitude (). Lightcurve inversion also modeled the body's shape and poles.
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The primary, component A, is an F-type subgiant star with a stellar classification of F8 IV, a star that has exhausted its core hydrogen and is evolving to become a red giant. The star was once thought to be a BY Draconis variable with the variable star designation MQ Ser, but has been found not to be. From observations made between 1975 and 1980, Bakos (1983) reported random, small brightness variations with an amplitude of less than 0.03 magnitude, plus three flare events that increased the brightness by 0.1 magnitudes.
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It adds a smoother circuit like the one in the radar receiver, which creates an amplitude modulated signal output. This output is then inverted and sent into the gain control. The result is an output signal that is strong when the radar signal is weak, and weak when it is strong. Depending on the exact strength of the signals, when this mixes with the radar's own signal at the radar receiver, the result is either a nearly flat smoothed curve, or one that is the inverse of the radar's curve.
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In January 2009, a rotational lightcurve of Poësia was obtained from photometric observations by Robert Stephens at the Santana Observatory and Goat Mountain Astronomical Research Station in California. Lightcurve analysis gave an exceptionally long rotation period of hours with a brightness amplitude of magnitude (). A few weeks later, Gary A. Vander Haagen at Stonegate Observatory determined an ambiguous period of 73.5 or 102.9 hours with an amplitude of magnitude (), while René Roy measured a tentative period of 48 hours (). With a best-rated period of 108.5 hours, Poësia is a slow rotator.
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In April 2011, a rotational lightcurve of Jucunda was obtained from photometric observations by Robert Stephens at the Santana Observatory and Goat Mountain Astronomical Research Station in California. Lightcurve analysis gave a rotation period of hours with a brightness amplitude of magnitude (). Observations in March 2011, by Luca Strabla, Ulisse Quadri and Roberto Girelli at Bassano Bresciano Observatory gave a period of hours with an amplitude of magnitude (). Additional period determinations of and were made by Eric Barbotin and Raoul Behrend in November 2019, and by Pierre Antonini in March 2011 ().
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In October 2010, a rotational lightcurve of Ilsebill was obtained from photometric observations by Zachary Pligge, Ben Hall and Richard Ditteon at the U.S. Oakley Observatory in Indiana. Lightcurve analysis gave a well-defined rotation period of hours with a brightness variation of magnitude (). In September 2010, a similar, though lower rated period of hours with an amplitude of was determined by astronomers at the Palomar Transient Factory in California (). A modeled lightcurve using photometric data from the Lowell Photometric Database and from the Wide-field Infrared Survey Explorer (WISE) was published in 2018.
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Several rotational lightcurves form photometric observations have been obtained for this body. In 1999, Czech astronomer Petr Pravec constructed a lightcurve, that rendered a rotation period of hours and a brightness variation of 0.72 in magnitude (). In March 2006, observations by astronomer David Polishook from the ground-based Wise Observatory, Israel, gave a rotation period of and amplitude of 0.70 mag (), and in November 2011, American astronomer Brian Warner at the Palmer Divide Observatory, Colorado, obtained the first well-defined period of hours with an amplitude of 0.50 mag ().
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French amateur astronomer René Roy obtained the first rotational lightcurve of Heckmann in September 2005. It gave a rotation period of 12.05 hours with a brightness variation of 0.06 in magnitude (). A more refined lightcurve with a period of 14.893 hours and an amplitude of 0.16 magnitude was obtained by Australian amateur astronomer David Higgins at the Hunters Hill Observatory and collaborating stations in March 2008 (). In September 2013, photometric observations at the Palomar Transient Factory, California, gave a low rated lightcurve with a similar period of 14.9042 hours ().
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In September 2012, a rotational lightcurve of Boucolion was first obtained from photometric observations by astronomers at the Palomar Transient Factory (PTF) in California. Lightcurve analysis gave a rotation period of 16.150 and 16.177 hours with a brightness amplitude of 0.23 and 0.25 magnitude in the R- and S-band, respectively (). A more refined, alternative period solution of hours with an amplitude of 0.21 magnitude was measured by Robert Stephens at the Center for Solar System Studies in January 2015 (). The result seems to be a 1:2 alias, i.e.
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Lightcurve-based 3D-model of Danzig In November 1988, Polish astronomer Wiesław Wiśniewski obtained a rotational lightcurve of Danzig from photometric observations. It gave a well-defined rotation period of hours with a brightness variation of 0.92 magnitude (). In October 2002, another lightcurve obtained by Italian and French amateur astronomers Silvano Casulli and Laurent Bernasconi gave a concurring period of hours and an amplitude of 0.81 magnitude (). While Danzig has an average rotation period, it has a high brightness variation, which indicates that the body has a non- spheroidal shape.
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In February 1992, a rotational lightcurve of Cebriones was obtained from photometric observations by Stefano Mottola and Anders Erikson using the now decommissioned ESO 1-metre telescope at La Silla Observatory in Chile. Lightcurve analysis gave a rotation period of 20.05 hours with a brightness variation of 0.22 magnitude (), superseding a previous measurement of a fragmentary lightcurve that gave 3.8 hours only (). In May 2008 and September 2010, observations by Brian A. Skiff and Adrián Galád gave a concurring period of 20.081 and 20.5 hours with an amplitude of 0.22 and 0.13, respectively ().
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Between January and March 2012, photometric observations for this asteroid were made by a team led by Petr Pravec at Ondřejov Observatory, Czech Republic. The three obtained rotational lightcurves gave an identical period of hours with a brightness variation of 0.55, 0.64 and 0.65 in magnitude, respectively (). Previously, in 2008, a lightcurve was obtained from observations at the Simeiz Observatory and the Chuguev Observing Station () in Ukraine, as well as at Maidanak Observatory in Uzbekistan. It also gave a period of 11.131 hours with an amplitude of 0.85 in magnitude, which implies an elongated shape ().
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In Summer 1986, the first photometric observations of Anchises were taken with the 0.9-meter telescope at the Cerro Tololo Observatory in Chile. Lightcurve analysis gave a well defined rotation period of 11.60 hours with a notably wide brightness variation of 0.57 magnitude (). Between January 2016, and December 2017, three more rotational lightcurves were obtained by American photometrist Robert Stephens at the Center for Solar System Studies in California. They gave a concurring period of 11.595, 11.596 and 11.599 hours with an amplitude between 0.34 and 0.73 magnitude ().
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In May 2002, a first rotational lightcurve of Bridges was obtained from photometric observations by French amateur astronomers René Roy and Laurent Bernasconi. Lightcurve analysis gave a well-defined rotation period of 3.6941 hours with a brightness variation of 0.24 magnitude (). A large number of observations have followed since 2006, when a satellite in orbit of Bridges was discovered (see below). Between 2007 and 2012, several observation by astronomers Petr Pravec and gave a period between 3.57459 and 3.5754 hours with an amplitude between 0.18 and 0.29 magnitude ().
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In October 2010, a rotational lightcurve of Birgitta was obtained from photometric observations by American astronomer Brian Skiff. Lightcurve analysis gave a well-defined rotation period of 8.994 hours with a brightness amplitude of 0.18 magnitude (). The result supersedes a previous observation by the discoverer Claes-Ingvar Lagerkvist from the 1970s, which showed a period of 9.02 hours and an amplitude of 0.4 magnitude (). In December 2014, astronomers at the Palomar Transient Factory in California measured as similar period of 8.97 hours with a brightness variation of 0.32 magnitude ().
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In August 2010, a rotational lightcurve of Polites was obtained from photometric observations over five nights by Linda French at the Cerro Tololo Inter-American Observatory in Chile. Lightcurve analysis gave a tentative rotation period of 9.21 hours with a low brightness variation of 0.09 magnitude (). Follow-up observations on a yearly basis by Robert D. Stephens and Daniel Coley at the Center for Solar System Studies gave several lightcurves during 2013–2018. The best-rated one from January 2016 gave a period of hours and an amplitude of 0.15 magnitude ().
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In the 1980s, a rotational lightcurve of Pandarus was obtained from photometric observations by Linda French using the SMARTS 0.9-meter reflector at Cerro Tololo Inter-American Observatory in Chile. Lightcurve analysis gave a well- defined rotation period of 8.480 hours with a brightness variation of 0.58 magnitude (), indicative of a non-spheroidal shape. In 2015 and 2017, Robert Stephens and Daniel Coley at the Center for Solar System Studies in California, measured two concurring periods of 8.461 and 8.470 hours with an amplitude of 0.49 and 0.65 magnitude, respectively ().
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In February 2005, a rotational lightcurve of Kustaanheimo was obtained from photometric observations by American astronomer John Menke at his Menke Observatory in Barnesville, Maryland (). Lightcurve analysis gave a rotation period of 4.286 hours with a brightness variation of 0.25 magnitude (). One month later, another well- defined lightcurve by French amateur astronomer Laurent Bernasconi gave a period of 4.302 hours and an amplitude of 0.23 magnitude (). In April 2016, Petr Pravec obtained an intermediary period of 4.3 hours with a brightness variation of 0.29 at the Ondřejov Observatory ().
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Three different rotational lightcurves of Kugultinov were obtain from photometric observations. The first, fragmentary lightcurve by Roberto Crippa and Federico Manzini in December 2013, gave a rotation period of 10 hours with a brightness variation of magnitude (). In April 2015, the result was superseded by observations made by Kim Lang at the Klokkerholm Observatory in Denmark, and by a team at the U.S. University of Maryland using the iTelescope network, obtaining a period of () and hours () with an amplitude of 0.23 and 0.19, respectively. CALL considers the shorter period solution the better result.
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In July 2008, a rotational lightcurve was obtained from photometric by astronomer Brian D. Warner at his Palmer Divide Observatory in Colorado, United States. It gave a well-defined rotation period of 5.2974 hours with a brightness variation of 0.25 in magnitude (). Several lightcurves with a lower or unassessed quality have been obtained by astronomers Wiesław Z. Wiśniewski and Petr Pravec in the 1980s and 1990s. The most recent observation by Michael Lucas in February 2011, gave a period of 5.317 hours with an amplitude of 0.33 magnitude ().
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In December 2005, a rotational lightcurve of Levasseur was obtained from photometric observations by Donald Pray at the Carbuncle Hill Observatory in collaboration with other European and American observers. Lightcurve analysis gave a rotation period of hours with a brightness variation of magnitude (). In April 2010, two nearly identical periods were found by David Higgins at the Hunters Hill Observatory in Australia and by Petr Pravec and collaborators at the Ondřejov Observatory in the Czech Republic. Their analysis gave a period of and hours with an amplitude of 0.13 and 0.09, respectively ().
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The so-far best rated rotational lightcurve of Latvia was obtained by the "Spanish Photometric Asteroid Analysis Group" (OBAS) in September 2015. Lightcurve analysis gave it a rotation period of 9.55 hours with a brightness variation of 0.23 magnitude (). Previous photometric observations by James W. Brinsfield at Via Capote Observatory and French amateur astronomer Laurent Bernasconi gave a period of 9.552 and 9.644 hours with an amplitude of 0.10 and 0.21 magnitude, respectively (). The first rotational lightcurve obtained by Richard P. Binzel in the 1980s gave a twice a long period solution of 18 hours ().
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In August 1995, a rotational lightcurve of Meges was obtained by ESO astronomers Stefano Mottola and Hans-Josef Schober using the Bochum 0.61-metre Telescope at La Silla Observatory in Chile. Lightcurve analysis gave a well-defined rotation period of 14.250 hours with a brightness variation of 0.13 magnitude (). Photometric observation of this asteroid by Robert Stephens and Daniel Coley at the Center for Solar System Studies during 2016 and 2017, gave two lightcurves with a concurring period of 14.266 and 14.285 hours and an amplitude of 0.27 and 0.44, respectively ().
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PKS 1302-102 is a quasar in the Virgo constellation, located at a distance of approximately 1.1 Gpc (around 3.5 billion light-years). It has an apparent magnitude of about 14.9 mag in the V band with a redshift of 0.2784. The quasar is hosted by a bright elliptical galaxy, with two neighboring companions at distances of 3 kpc and 6 kpc. The light curve of PKS 1302-102 appears to be sinusoidal with an amplitude of 0.14 mag and a period of 1,884 ± 88 days, which suggests evidence of a supermassive black hole binary.
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The movement of the object causes a shift in the phase of the signal, which cannot be identified directly by an optical receiver: to do this it is first necessary to transform the phase modulation into an amplitude modulation (in this case, in a modulation of luminous intensity ). Ultrasound detection can therefore be divided into 3 steps: the conversion from ultrasound to phase-modulated optical signal, the transition from phase modulation to amplitude and finally the reading of the amplitude modulated signal with consequent conversion into an electrical signal.
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The discovery of the planet was announced in August 2016. The planet was found using the radial velocity method, where periodic Doppler shifts of spectral lines of the host star suggest an orbiting object. From these readings, the radial velocity of the parent star relative to the Earth is varying with an amplitude of about 1.4 metres (4.5 feet) per second. According to Guillem Anglada‐Escudé, its proximity to Earth offers an opportunity for robotic exploration of the planet with the Starshot project or, at least, "in the coming centuries".
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The fundamental zero-order Bessel beam has an amplitude maximum at the origin, while a high-order Bessel beam (HOBB) has an axial phase singularity along the beam axis; the amplitude is zero there. HOBBs can be of vortex (helicoidal) or non-vortex types. X-waves are special superpositions of Bessel beams which travel at constant velocity, and can exceed the speed of light. Mathieu beams and parabolic (Weber) beams are other types of non-diffractive beams that have the same non-diffractive and self-healing properties of Bessel beams but different transverse structures.
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In October 2001, a first rotational lightcurve of Villigera was obtained by astronomer Robert Koff at Thornton Observatory () in Colorado. Light curve analysis gave a well-defined rotation period of 7.830 hours with a brightness variation of 0.39 magnitude (). Photometric observations by astronomers René Roy, Raoul Behrend and Pierre Antonini in February 2006, gave a concurring period of 7.834 hours and an amplitude of 0.36 magnitude (). In 2016, a modeled lightcurves using photometric data from various sources, rendered an identical period of 7.830 and a spin axis of (3.0°, 63°) in ecliptic coordinates.
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In August 2012, two rotational lightcurves of Sieböhme were obtained at the Palomar Transient Factory in California, and by Italian astronomer Albino Carbognani. These lightcurves gave a rotation period of 56.8129 and 56.81 hours with a brightness variation of 0.44 and 0.45 magnitude, respectively (). One month later, photometric observations by amateur astronomer Pierre Antonini gave a period of 56.65 hours and an amplitude of 0.47 magnitude (). As most minor planets rotate within 2 to 20 hours around their axis, Sieböhme has a relatively long period, despite not being a slow rotator.
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We have seen above that the Weierstrass transform of cos(bx) is e−b2 cos(bx), and analogously for sin(bx). In terms of signal analysis, this suggests that if the signal f contains the frequency b (i.e. contains a summand which is a combination of sin(bx) and cos(bx)), then the transformed signal F will contain the same frequency, but with an amplitude multiplied by the factor e−b2. This has the consequence that higher frequencies are reduced more than lower ones, and the Weierstrass transform thus acts as a low-pass filter.
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In April 2017, a rotational lightcurve of Larissa was obtained from photometric observations by American astronomers Brian Warner and Robert Stephens at the Center for Solar System Studies () in California. Lightcurve analysis gave a well-defined rotation period of 6.514 hours with a brightness variation of 0.12 magnitude (). In May 2010, a lightcurve form the Oakley Southern Sky Observatory () in Australia, gave a concurring period of 6.516 hours with an amplitude of 0.20 magnitude (). Another period of 6.520 hours (Δ0.12 mag) was measured at the Palomar Transient Factory in October 2012 ().
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In February 2009, a rotational lightcurve of China was obtained from photometric observations by Kenneth T. Menzies at the Tigh Speuran Observatory in Massachusetts, United States. Lightcurve analysis gave a well-defined rotation period of 5.367 hours with a brightness variation of 0.38 magnitude (). In October 2013, Robert Stephens measured a similar period of 5.45 hours and an amplitude of 0.62 magnitude at the Center for Solar System Studies in California (). Published in 2016, an additional lightcurve was modeled from photometric data obtained by a large international collaboration of astronomers.
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The star is receding from the Earth with a heliocentric radial velocity of +15 km/s. This is an A-type main sequence star with a stellar classification of A9 V. It is a Delta Scuti variable with a variability period of 0.0676 days and an amplitude of 0.010 in magnitude. The star is around a billion years old with 1.74 times the mass of the Sun and 2.32 times the Sun's radius. The star is radiating 15 times the luminosity of the Sun from its photosphere at an effective temperature of 7,430 K.
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The magnitude 5.08 primary member, designated component A, is a single-lined spectroscopic binary system in a circular orbit with a period of 3.7887 days. The visible member has a stellar classification of A9 IV or A V, depending on the source, and is a Delta Scuti variable with an amplitude of 0.08 magnitude and a period of 2.11 hours. It is 609 million years old with 1.64 times the mass of the Sun. Component B lies about to the north of the primary and is merely a visual companion.
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A rotational lightcurve of Hirayama was obtained at the Menke Observatory in February 2002. It showed a periodicity of hours, during which time the brightness of Hirayama varies by in magnitude (). At the same time, photometric observations by astronomers Roberto Crippa and Federico Manzini gave a rotation period of 22.37 hours and a brightness variation of 0.47 magnitude (). These results supersede an observation from January 2005, by Hiromi and Hiroko Hamanowa at their Hamanowa Astronomical Observatory, Japan, that gave a shorter period of 13.59 hours with an amplitude of 0.57 magnitude.().
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Eighty Mile Beach lies along the thin south-western extension of the Dampierland bioregion (shown in red) Eighty Mile Beach lies in the Shire of Broome in the Kimberley region of Western Australia, in the Dampierland bioregion. It extends south-west from Cape Missiessy in a shallow curve to Cape Keraudren , with its midpoint at . The beach is about 100 m wide and has a gentle gradient. It consists of sand with a high proportion of shelly material, and experiences a very large tidal range with an amplitude of up to 9 m.
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In July 1994, a first rotational lightcurve of Thersites was obtained from photometric observations by Italian astronomer Stefano Mottola using the former Dutch 0.9-metre Telescope at ESO's La Silla Observatory in northern Chile. Lightcurve analysis gave a rotation period of hours with a brightness variation of magnitude (). The best-rated lightcurve by Robert Stephens at the Center for Solar System Studies from June 2016 gave a period of 10.48 hours and an amplitude of 0.27 magnitude (). Follow-up observation in 2017 gave a similar period of 10.412 hours ().
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In June 2016, observation by Brian Warner at the Palmer Divide Station at the Center for Solar System Studies in California, gave an exceptionally long period hours and an amplitude of magnitude (), which makes it a slow rotator. The observations also indicated that Idomeneus is a binary asteroid with a minor- planet moon in its orbit. The satellite's orbital period is hours, or alternatively, hours with a brightness variation of 0.14 magnitude. However, the results are tentative and have not been published in any journal as of 2018.
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In December 2010 and April 2014, follow-up observations by Daniel Coley in collaboration with Robert Stephens at the Center for Solar System Studies and the Goat Mountain Astronomical Research Station rendered a period of 8.64 and 8.45 hours and an amplitude of 0.15 magnitude (). The result shows that Binzel's first measurement was probably an alternative period solution (i.e. twice the actual period). In February 2013, Michael Alkema at the Elephant Head Observatory in Arizona reported a concurring period of 8.639 hours with a brightness variation of 0.08 magnitude ().
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In February 1993, a rotational lightcurve of ' was obtained from photometric observations by Italian astronomers Stefano Mottola and Mario Di Martino, using the ESO 1-metre telescope at ESO's La Silla site, Chile. Lightcurve analysis gave a rotation period of 6.553 hours with a brightness variation of 0.23 magnitude (). In January 2015, and February 2016, observations by Robert Stevens and Daniel Coley at the Center for Solar System Studies in California gave two concurring periods of and hours and an amplitude of 0.31 and 0.20 in magnitude, respectively ().
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In November 2011, a rotational lightcurve of Lydina was obtained from photometric observations by Robert Stephens at his Santana Observatory in California. Lightcurve analysis gave a well-defined rotation period of 11.680 hours with a brightness variation of 0.22 magnitude (). Observations at the Italian Bassano Bresciano Observatory in December 2011 measured a concurring period 11.674 with an amplitude of 0.30 magnitude (). A previous observations at the Pico dos Dias Observatory , Brasil, gave a period of 15.69 hours, which Stephens interpreted as a 4:3-alias period solution of his results.
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In September 2009, two rotational lightcurves of Nanna were obtained by American astronomer Brian Warner from photometric observations at his Palmer Divided Observatory in Colorado. The first lightcurve analysis gave a rotation period of 18.54 hours with a brightness variation of 0.12 magnitude (), while the second lightcurve was ambiguous giving a period of 25.80 and 12.90 hours, respectively, and an amplitude of 0.15 (). These results supersede a fragmentary lightcurve taken by French amateur astronomers Federico Manzini, Laurent Bernasconi and René Roy from August 2004, which gave a period of 15.6 hours ().
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A faint ring arc, first detected in September 2006, covering a longitudinal extent of about 10 degrees is associated with the moon Methone. The material in the arc is believed to represent dust ejected from Methone by micrometeoroid impacts. The confinement of the dust within the arc is attributable to a 14:15 resonance with Mimas (similar to the mechanism of confinement of the arc within the G ring). Under the influence of the same resonance, Methone librates back and forth in its orbit with an amplitude of 5° of longitude.
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BD Phoenicis is a Lambda Boötis star, an uncommon type of peculiar stars that have very low abundances of iron-peak elements. In particular, BD Phoenicis has near-solar carbon and oxygen content, but its iron abundance is only 4% the solar value. BD Phoenicis is also a pulsating variable of Delta Scuti type, varying its apparent magnitude between 5.90 and 5.94. A study of its light curve detected seven pulsation periods that range from 50 to 84 minutes, the strongest one having a period of 57 minutes and an amplitude of 9 milli- magnitudes.
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In September 1996, observations by Stefano Mottola using the now decommissioned Bochum 0.61-metre Telescope at ESO's La Silla Observatory in Chile gave a rotation period of 18.22 hours with a brightness amplitude of 0.14 magnitude (). Between 2010 and 2015, refined photometric observations by Robert Stephens, Daniel Coley, Brian Warner and collaborators at the Center for Solar System Studies in Landers, California, gave three concurring periods of 18.14–18.216 hours and a brightness variation of 0.22–0.39 magnitude, with the best rated result of 18.192 hours and an amplitude of 0.22 magnitude ().
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Several rotational lightcurves were obtained for this asteroid from photometric observations. In September 2013, Italian astronomer Andrea Ferrero at the Bigmuskie Observatory in Mombercelli, Italy, derived a rotation period of hours with a brightness variation of 0.11 in magnitude (), while two month later, in November 2013, astronomer Brian A. Skiff obtained two lightcurves that both gave a period of 2.95 and an amplitude of 0.24 and 0.28 in magnitude, respectively (). The results supersede two older lightcurves from 1991 and 2002, that gave a period of and 6 hours, respectively ().
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In March 2011, photometric observations revealed that Soma is a synchronous binary asteroid with a minor-planet moon orbiting it every 17.915 hours. The system has a secondary-to-primary mean-diameter ratio of 0.25, which means that satellite's diameter measures approximately 25% of that of Soma (the primary), and translate into a diameter of 1.75 kilometers. The observations also gave a refined rotation period for Soma of 2.73325 hours and an amplitude of 0.07 magnitude (). The system has an absolute magnitude of 12.53, and a phase slope parameter (G) of 0.27.
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Tau2 Hydrae is a probable astrometric binary star system in the equatorial constellation of Hydra. Based upon an annual parallax shift of 6.30 mas as seen from Earth, it is located around 520 light years from the Sun. The brighter component is visible to the naked eye with an apparent visual magnitude of +4.56. The primary member, component A, is an A-type main sequence star with a stellar classification of A3 V. It is a suspected variable of unknown type, with an amplitude of 0.06 in visual magnitude.
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On the other hand, in medium wave and short wave broadcasting, standard AM with the full carrier allows for reception using inexpensive receivers. The broadcaster absorbs the extra power cost to greatly increase potential audience. An additional function provided by the carrier in standard AM, but which is lost in either single or double-sideband suppressed-carrier transmission, is that it provides an amplitude reference. In the receiver, the automatic gain control (AGC) responds to the carrier so that the reproduced audio level stays in a fixed proportion to the original modulation.
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For instance, consider a damped harmonic oscillator such as a pendulum, or a resonant L-C tank circuit. If the pendulum has been at rest and we were to strike it with a hammer (the "impulse"), setting it in motion, it would swing back and forth ("resonate"), say, with an amplitude of 10 cm. After 10 minutes, say, the pendulum would still be swinging but the amplitude would have decreased to 5 cm, half of its original amplitude. After another 10 minutes its amplitude would be only 2.5 cm, then 1.25 cm, etc.
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It contains numerous trenches and irregular peaks, which usually have an amplitude of less than 100 metres, but can reach up to 400 metres. They are covered with a mixture of gravel, sand, and mud, and the trenches are used by fish as spawning grounds. Deeper into the sea, there are two deep basins separated by a low ridge (its deepest point at 3,000 m) between the Vøring Plateau and Jan Mayen island. The southern basin is larger and deeper, with large areas between 3,500 and 4,000 metres deep.
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In October 2017, a rotational lightcurve of Cupido was obtained from photometric observations by American astronomer Frederick Pilcher in collaboration with Vladimir Benishek at Belgrade Observatory and Daniel A. Klinglesmith at Etscorn Observatory . Lightcurve analysis gave a rotation period of hours with a brightness variation of magnitude (). The observations also showed that it is a tumbling asteroid, which wobbles on its non-principal axis rotation. During the same opposition, Tom Polakis at the Command Module Observatory also observed the asteroid and measured a period of hours and an amplitude of magnitude ().
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Additional observations by Christophe Demeautis in September 2017, and by Bruno Christmann in April 2020, gave a period of () and () hours with an amplitude of and magnitude, respectively (). In 2016, a modeled lightcurve rendered a concurring sidereal period of hours using data from the Uppsala Asteroid Photometric Catalogue, the Palomar Transient Factory survey, and individual observers, as well as sparse-in-time photometry from the NOFS, the Catalina Sky Survey, and the La Palma surveys . The study also determined two spin axes of (83.0°, 40.0°) and (275.0°, 21.0°) in ecliptic coordinates (λ, β).
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In March 2018, a rotational lightcurve of Nora was obtained from photometric observations by Tom Polakis at the Command Module Observatory in Arizona. Lightcurve analysis gave a rotation period of hours with a low brightness variation of magnitude (). The result supersedes previous observations by European astronomers at the La Silla, Haute Provence and Hoher List observatories during the 1990s which gave two periods of and with an amplitude of and magnitude, respectively (). In April 2007, French astronomer Arnaud Leroy determined a period of and a brightness variation of 0.01 magnitude ().
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In 2013, a rotational lightcurve for this asteroid was obtained from photometric observations made by astronomer Anna Marciniak at Poznań Observatory, Poland. It gave a rotation period of hours with a brightness variation of 0.22 in magnitude (), superseding a period from in 2000, obtained at the Californian Santana Observatory (), which gave a slightly longer period of hours and an amplitude of 0.11 (). Between 2004 and 2006, three more lightcurves were constructed from photometric observations, but they were all fragmentary and based on results with less than full coverage ().
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Located at an estimated distance of , this is a close binary system with a degenerate white dwarf primary in orbit with a cool red dwarf secondary over a period of 0.145143 days. Matter from the red dwarf is being drawn off onto an accretion disk orbiting the white dwarf. The mean brightness of the system varies with an amplitude of 0.5 magnitude from day to day. The observational data shows a general period of 0.037 days, which may be related to the rotation period of the white dwarf component.
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At an age of just 13.4 million years, Sigma Lupi is spinning with a projected rotational velocity of 68 km/s giving it a rotation period of 3.02 days. A magnetic field has been detected with a polar field strength of around 500 G, which is varying longitudinally with an amplitude of around 100 G. The star has an estimated nine times the mass of the Sun and 4.8 times the Sun's radius. It is radiating 5,754 times the solar luminosity from its outer atmosphere at an effective temperature of around 23,000 K.
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Their mean solution of for Huya's rotation period appeared consistent with previous photometric observations, with an amplitude less than 0.1 magnitudes. However, the rotation period determined by Ortiz was later determined to be an alias of Huya's brightness variability. In 2014, Thirouin suggested a shorter fragmentary rotation period of 5.28 hours, tentatively determined from short- term photometric observations conducted in 2010 through 2013. Like the former rotation period inferred by Ortiz, the latter period obtained by Thirouin was based on fragmentary photometric data and may be erroneous by a factor of 30 percent or more.
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7 Cephei is a single star located approximately 820 light years away, in the northern circumpolar constellation of Cepheus. It is visible to the naked eye as a dim, blue-white hued star with an apparent visual magnitude of 5.42. This is a B-type main-sequence star with a stellar classification of B7 V. It is a candidate variable star with an amplitude of 9 micromagnitudes and a period of . This object has 4.5 times the mass of the Sun and about three times the Sun's radius.
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This is a B-type main sequence star with a stellar classification of B3/4 V. It is a microvariable with a period of 10.7 hours and an amplitude of 0.0046 in magnitude. With an age of just 44 million years, the star is spinning with a projected rotational velocity of 166 km/s. This is giving the star an oblate shape with an equatorial bulge that is an estimated 6% larger than the polar radius. It has an estimated 4.66 times the mass of the Sun and about 3.4 times the Sun's radius.
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The average of the true solar day during the course of an entire year is the mean solar day, which contains . Currently, each of these seconds is slightly longer than an SI second because Earth's mean solar day is now slightly longer than it was during the 19th century due to tidal friction. The average length of the mean solar day since the introduction of the leap second in 1972 has been about 0 to 2 ms longer than .Leap seconds Random fluctuations due to core-mantle coupling have an amplitude of about 5 ms.
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The star has a relatively high proper motion, traversing the celestial sphere at the rate of /yr. Based upon a stellar classification of F0 IV, this is an aging F-type subgiant star that has consumed the hydrogen at its core. It is spinning rapidly with a projected rotational velocity of 165 km/s, giving it an oblate shape with an equatorial bulge that is estimated to be 8% larger than the polar radius. CL Dra is a Delta Scuti variable, changing brightness with an amplitude of 0.010 magnitude over a period of .
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It is a candidate member of the Hyades supercluster and has a peculiar velocity of 9.2 km/s. The visible component of this system is an evolved K-type giant star with a stellar classification of K4 III. It is a periodic variable with a frequency of a cycle every 10.64724 days and an amplitude of 0.0041 in magnitude. The star has an estimated 37 times the radius of the Sun and is radiating 318 times the Sun's luminosity from its enlarged photosphere at an effective temperature of about 4,105 K.
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Warren Grill and J. Thomas Mortimer, may be observed in the adjacent image. Building upon this, a stimulus with two depolarizing prepulses, each of an amplitude slightly below the threshold current (at the time of delivery), should increase the radii of influence for nearby nerve fiber inactivation and distant nerve fiber excitation. Typically, nerve fibers of a larger diameter may be activated by single-pulse stimuli of a lower intensity, and thus may be recruited more readily. However, DPPs have demonstrated the additional capability to invert this recruitment order.
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S+ being on for the half-bridge corresponds to S1+ and S2- being on for the full-bridge. Similarly, S- being on for the half-bridge corresponds to S1- and S2+ being on for the full bridge. The output voltage for this modulation technique is more or less sinusoidal, with a fundamental component that has an amplitude in the linear region of less than or equal to one '. Unlike the bipolar PWM technique, the unipolar approach uses states 1, 2, 3 and 4 from Table 2 to generate its AC output voltage.
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Other software, like HFSS can also compute the near field. The far field radiation pattern may be represented graphically as a plot of one of a number of related variables, including; the field strength at a constant (large) radius (an amplitude pattern or field pattern), the power per unit solid angle (power pattern) and the directive gain. Very often, only the relative amplitude is plotted, normalized either to the amplitude on the antenna boresight, or to the total radiated power. The plotted quantity may be shown on a linear scale, or in dB.
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Features along the coast push the current further off shore and if there is a strong northerly wind, it will push the current even further off shore, allowing deep water to rise up the coast, bringing nutrients up to the surface. The EAC experiences seasonal variations. It tends to be strongest in the summer, with an amplitude flow around 36.3 Sv. It is its weakest during the winter months flowing at a rate around 27.4 Sv. Over the past 50–60 years the EAC has shifted. The south Tasman Sea has become warmer and saltier from 1944–2002.
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The diver's speech is picked up by the microphone and converted into a high frequency sound signal transmitted to the water by the omnidirectional transducer. The signal can bounce off the bottom and surface and other obstructions, which can extend the range around obstructions, but will also degrade the signal due to interference effects caused by varying path lengths of different routes. When a receiving transducer picks up the signal, the ultrasonic signal is converted to an amplitude modulated electrical signal, amplified and converted to sound by the earphone. The through-water communications sets carried by the divers are battery powered.
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In May 2010, a rotational lightcurve of Mellena was obtained from photometric observations by Robert Stephens at the Santana and GMARS observatories in California. Lightcurve analysis gave a well-defined rotation period of hours with a brightness variation of magnitude (). Subsequent observations were taken by Andrea Ferrero at the Bigmuskie Observatory in Mombercelli, Italy (), and Larry Owings at the Barnes Ridge Observatory in California in June 2010 (), as well as by Albino Carbognani Astronomical at the OAVdA Observatory in July 2010 (). These observations gave a concurring period of (), () and () hours with an amplitude of (), () and () magnitude, respectively.
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In April 2008, a rotational lightcurve of Hildegard was obtained from photometric observations by Australian amateur astronomer David Higgins. Lightcurve analysis gave a well- defined rotation period of hours with a brightness variation of magnitude (). Previously in June 1999, observations by Brian Warner at his Palmer Divide Observatory in Colorado only gave a period of above 24 hours and an amplitude larger than 0.3 magnitude (). Asteroid's with a rotation period near 24 hours are difficult to observe, since full coverage can not be obtained by a few consecutive nights of observation from a single observatory alone, due to Earth's nearly synchronous rotation.
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A three-dimensional model of 807 Ceraskia based on its light curve In October 2017, a rotational lightcurve of Ceraskia was obtained from photometric observations by Matthieu Conjat at Nice Observatory in France. Lightcurve analysis gave a well-defined rotation period of hours with a brightness variation of magnitude (). The result supersedes previous observations by Richard Binzel in April 1983 and by astronomers at the Palomar Transient Factory in California on October 2012, which gave a period of and hours with an amplitude of and magnitude, respectively (). Lightcurve inversion also modeled the body's shape and poles.
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In August 2000, a rotational lightcurve of Camelia was obtained from photometric observations by Brian Warner at the Palmer Divide Observatory in Colorado. The originally published lightcurve analysis gave a wrong rotation period of hours with a brightness variation of magnitude (). In July 2010, and with the availability of improved analysis tools and techniques along with the experience gained over more than a decade, Warner reviewed and recalibrated the original data set and determined a period of at least hours with an amplitude of more than (). With such a long period, Camelia is a slow rotator.
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In December 2009, a rotational lightcurve of Petunia was obtained from photometric observations by Robert Stephens at Santana Observatory and Goat Mountain Astronomical Research Station in California. Lightcurve analysis gave a long rotation period of hours with a brightness variation of magnitude (). Astronomers at the Palomar Transient Factory in California measured a period of hours and an amplitude of 0.30 magnitude in August 2013 (), while observations by Italian amateur astronomers Roberto Crippa and Federico Manzini at the Sozzago Astronomical Station in April 2006 were of poor quality (). A modeled lightcurve using photometric data from the Lowell Photometric Database was published in 2016.
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This variation is due to the apparent precession of the rotating Earth through the year, as seen from the Sun at solar midday. In terms of the equation of time, the inclination of the ecliptic results in the contribution of a sine wave variation with an amplitude of 9.87 minutes and a period of a half year to the equation of time. The zero points of this sine wave are reached at the equinoxes and solstices, while the extrema are at the beginning of February and August (negative) and the beginning of May and November (positive).
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Contributions from paths wildly different from the classical trajectory may be suppressed by interference (see below). Feynman showed that this formulation of quantum mechanics is equivalent to the canonical approach to quantum mechanics when the Hamiltonian is at most quadratic in the momentum. An amplitude computed according to Feynman's principles will also obey the Schrödinger equation for the Hamiltonian corresponding to the given action. The path integral formulation of quantum field theory represents the transition amplitude (corresponding to the classical correlation function) as a weighted sum of all possible histories of the system from the initial to the final state.
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In November 2000, a rotational lightcurve of Griqua was obtained from photometric observations by Colin Bembrick at the Mount Tarana Observatory in Australia. Lightcurve analysis gave a well-defined rotation period of 6.907 hours with a brightness variation of 0.25 magnitude (). In 2009, follow-up observations by Jean and Milan Strajnic , Alain Klotz and Raoul Behrend as well as observations in the S-band by astronomers at the Palomar Transient Factory in California gave a concurring period of 6.891 and 6.9 hours with an amplitude of 0.23 and 0.24 magnitude, respectively (). The result supersedes a measurement of 7 hours made in the 1970s ().
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In February 1994, a rotational lightcurve of Deikoon was obtained from six nights of photometric observations by Stefano Mottola and Anders Erikson using the ESO 1-metre telescope at the La Silla Observatory in Chile. The irregular lightcurve showed a rotation period of hours and a low brightness variation of 0.07 magnitude (). In March 2007, a refined period of hours with an amplitude of 0.14 magnitude was obtained by Lawrence Molnar at Calvin College, remotely operating the 0.4-meter telescope at the Calvin-Rehoboth Robotic Observatory in New Mexico (). A low brightness amplitude is indicative of a spherical rather than elongated shape.
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In April 2006, a rotational lightcurve of Dysona was obtained by Julian Oey at Leura Observatory () in Australia. Lightcurve analysis gave a rotation period of 8.6080 hours with a brightness variation of 0.24 magnitude (), superseding photometric observations by Jean-Gabriel Bosch and Laurent Brunetto in October 2010, who measured a period of 8.355 hours and an amplitude of 0.25 magnitude (). In 2016, a modeled lightcurve using data from UAPC, the Palomar Transient Factory survey, and individual observers, gave a concurring period of 8.60738 hours as well an astronomical pole of (125.0°, −68.0°) in ecliptic coordinates (λ, β).
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A rotational lightcurve of Beckman was obtained from photometric observations by Polish astronomer Wiesław Wiśniewski during 1986–1987. Lightcurve analysis gave a well-defined rotation period of hours with a brightness amplitude of 0.16 magnitude (). Observations by Daniel Klinglesmith at Etscorn Campus Observatory in November 2013, gave a period of 3.130 hours and an amplitude of 0.27 magnitude (). Serbian astronomer Vladimir Benishek at the Belgrade Astronomical Observatory measured a period of 3.125 hours in December 2017 (), and in March 2018, Robert Stephens at the Center for Solar System Studies in California determined a period of 3.113 ().
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American astronomer Richard Binzel obtained the first rotational lightcurve of Brenda in June 1984. It gave a rotation period of 19.46 hours with a brightness variation of 0.16 magnitude (). In June 2006, a period of with an amplitude of 0.26 magnitude was derived from photometric observations made by French amateur astronomer René Roy (). According to the surveys carried out by the Infrared Astronomical Satellite IRAS, the Japanese Akari satellite, and NASA's Wide-field Infrared Survey Explorer with its subsequent NEOWISE mission, Brenda measures between 26.27 and 29.64 kilometers in diameter, and its surface has an albedo between 0.115 and 0.133.
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Photometric observations of McCleese by Brian Warner and René Roy in 2005 and 2007, gave three rotational lightcurves that had a rotation period between 7.2 and 28.8 hours with a brightness variation of 0.06 to 0.50 magnitude (). In June 2010, McCleese was again observed by Brian Warner at his Palmer Divide Observatory in Colorado, United States. By combining his data points with the previously obtained photometric data, he was able to derive a period of hours with an amplitude of 1.30 magnitude (). With a period of 418 hours, the body is one of the Top 100 slow rotators known to exist.
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In February 2006, a rotational lightcurve was obtained by American astronomer Brian Warner at his Palmer Divide Observatory () in Colorado. Lightcurve analysis gave a rotation period of 17.490 hours with a brightness variation of 0.50 in magnitude (). Photometric observations at the Palomar Transient Factory in February 2012, gave a period of 17.5226 hours and an amplitude of 0.49 magnitude (). In 2011, a modeled lightcurve using data from the Uppsala Asteroid Photometric Catalogue (UAPC) and other sources gave a period 17.5157 hours, as well as a spin axis of (22.0°, –76.0°; 167.0°, –40.0°) in ecliptic coordinates (λ, β) ().
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The primary component is an F-type main-sequence star with a stellar classification of F0 V. It is a Delta Scuti variable with an amplitude of 0.02 in magnitude and a frequency of 0.16 d−1. This star has about 1.94 times the mass of the Sun and 3.34 times the Sun's radius. It has a projected rotational velocity of 192 km s−1, for an estimated rotation period of 14.2 days. Extreme ultraviolet flares have been observed coming from this star's hot corona, and it is the second brightest X-ray source in the Hyades.
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In October 2003, a rotational lightcurve of Lucifer was obtained from photometric observations by American astronomer Brian Warner at his Palmer Divide Observatory in Colorado. Lightcurve analysis gave a well-defined rotation period of 13.056 hours with a brightness amplitude of 0.44 magnitude (). In January 2005, observations by astronomer Horacio Correia gave a concurring period of 13.054 hours and an amplitude of 0.22 magnitude (). In 2013, another lightcurve was obtained at the Palomar Transient Factory (), and a modeled lightcurve from various data sources, including the AstDyS database, gave another concurring period of 13.0536 hours and found a pole of (32.0°,17.0°).
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Single/Multi Channel Simulcast is the simultaneous transmission of an amplitude modulated and Digital Radio Mondiale (DRM) in the same (SingleChannel Simulcast - SCS) or a neighbouring channel (MultiChannel Simulcast - MCS). To produce this SCS multiplex signal, the initial carrier is modulated by the DRM signal using quadrature phase modulation. This FM signal is then modulated as if it were a normal AM carrier, thus producing two modes on the single signal. Clearly the advantage of this is that both DRM and analogue radios can receive a signal they can discriminate and demodulate, with little disadvantage to either mode.
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Several rotational lightcurves of Adams were obtained from photometric observations in 2010 and 2012. Best-rated lightcurve analysis gave a rotation period of hours with a brightness variation between 0.40 and 0.46 magnitude (). Additional photometric observations gave similar periods of 3.316, 3.27 and 3.560 hours with an amplitude of 0.60, 0.28 and 0.34, respectively (). According to the surveys carried out by the Japanese Akari satellite and NASA's Wide-field Infrared Survey Explorer with its subsequent NEOWISE mission, Adams measures between 10.1 and 13.5 kilometers in diameter and its surface has an albedo between 0.141 and 0.395.
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Photometric observations of Telamon by Stefano Mottola from August 1995 were used to build a lightcurve rendering a rotation period of 11.2 hours with a brightness variation of in magnitude (). In October 2010, another observation by Robert Stephens at the Goat Mountain Astronomical Research Station in California gave a period of 16.975 hours (). In August 2017, observations by the K2 mission of the Kepler spacecraft during Campaign 6 gave two periods of 11.331 and 22.613 hours with an amplitude of 0.06 and 0.07 magnitude, respectively (). The body is possibly of spherical shape as all lightcurves measured a very small variation in brightness.
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In April 2005, a rotational lightcurve of Crimea was obtained by American astronomer Robert Stephens at Santana Observatory in California. Lightcurve analysis gave a well-defined rotation period of 9.77 hours with a brightness variation of 0.30 magnitude (). Photometric observations by amateur astronomers Federico Manzini and Pierre Antonini in March 2014, gave a concurring period of 9.784 hours with an amplitude of 0.23 magnitude (). In addition, a modeled lightcurve using data from the Uppsala Asteroid Photometric Catalogue and other sources gave a period 9.7869 hours, as well as a spin axis of (12.0°, -73.0°) in ecliptic coordinates ().
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In January 2004, the best-rated rotational lightcurve of Mimi was obtained from photometric observations by astronomer John Menke at his Menke Observatory in Barnesville, Maryland (no obs. code). Lightcurve analysis gave a well-defined rotation period of 12.749 hours with a brightness amplitude of 0.72 magnitude (). Two other lightcurves gave a shorter period of 8.541 hours with an amplitude of 0.93 and 0.95 magnitude, respectively (). A 2016-published lightcurve, using modeled photometric data from the Lowell Photometric Database (LPD), gave a concurring period of 12.74557 hours, as well as a spin axis of (224.0°, −57.0°) in ecliptic coordinates (λ, β).
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Communication from the reader to the card uses an amplitude-shift keying with 10% or 100% modulation index. The data coding is: ;1 out of 4 pulse position modulation: 2 bits are coded as the position of a 9.44 μs pause in a 75.52 μs symbol time, giving a bit rate of 26.48 kilobits per second. The least-significant bits are sent first. ;1 out of 256 pulse position modulation: 8 bits are coded as the position of a 9.44 μs pause in a 4.833 ms symbol time, giving a bit rate of 1.65 kbit/s.
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In fact spin networks constitute a basis for all gauge invariant functions which minimize the degree of over-completeness of the loop basis, and for trivalent intersections eliminate it entirely. As mentioned above the holonomy tells you how to propagate test spin half particles. A spin network state assigns an amplitude to a set of spin half particles tracing out a path in space, merging and splitting. These are described by spin networks \gamma: the edges are labelled by spins together with `intertwiners' at the vertices which are prescription for how to sum over different ways the spins are rerouted.
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The Fourier transform is almost always computed using the fast Fourier transform (FFT) computer algorithm in combination with a window function. In the case of our square wave force, the first component is actually a constant force of 0.5 newton and is represented by a value at 0 Hz in the frequency spectrum. The next component is a 1 Hz sine wave with an amplitude of 0.64. This is shown by the line at 1 Hz. The remaining components are at odd frequencies and it takes an infinite amount of sine waves to generate the perfect square wave.
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In addition to the steady progressive motion (resulting in a full circle in about 25,700 years) the Sun and Moon also cause small periodic variations, due to their changing positions. These oscillations, in both precessional speed and axial tilt, are known as the nutation. The most important term has a period of 18.6 years and an amplitude of 9.2 arcseconds. In addition to lunisolar precession, the actions of the other planets of the Solar System cause the whole ecliptic to rotate slowly around an axis which has an ecliptic longitude of about 174° measured on the instantaneous ecliptic.
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In the 1990s, a rotational lightcurve of Richilde was first obtained from photometric observations by astronomers using the ESO 1-metre telescope at the La Silla Observatory in Chile. Lightcurve analysis gave a well-defined rotation period of 9.860 hours with a brightness variation of 0.32 magnitude (). In October 2006, a concurring period of 9.870 hours and an amplitude of 0.31 was measured by French amateur astronomer Raymond Poncy (). In 2011, a modeled lightcurve using data from the Uppsala Asteroid Photometric Catalogue (UAPC) and other sources gave a period 9.86687 hours, as well as a partial spin axis of (n.a.
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In May 1992, a rotational lightcurve of Eurybates was obtained from photometric observations by Stefano Mottola and Maria Gonano–Beurer using the now decommissioned ESO 1-metre telescope at La Silla Observatory in northern Chile. Lightcurve analysis gave a rotation period of 8.711 hours with a brightness variation of 0.20 magnitude (). In October 2010, photometric observations by American astronomer Robert Stephens at the Goat Mountain Astronomical Research Station in California gave a concurring period of 8.73 hours and an amplitude of 0.19 magnitude (). Eurybates has two determined spin axes at (143.0°, −45.0°) and/or (325.0°, –61.0°) in ecliptic coordinates (λ, β).
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In October 2009, a rotational lightcurve was obtained from photometric observations by astronomer Stefano Mottola at the Calar Alto Observatory in Spain. It gave a well-defined rotation period of hours with a brightness variation of 0.21 in magnitude (), superseding a period of 13.52 hours and an amplitude of more than 0.20 previously measured with the ESO 1-metre telescope at La Silla Observatory in May 1991 (). In August 2015, photometric observations of 1986 WD by the Kepler space observatory during its K2 mission gave a concurring period of 13.475 and 13.49 hours with a brightness amplitude of 0.18 and 0.17 magnitude observations ().
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87–89 both of which reported upon the observation of a 160-minute solar oscillation with an amplitude of approximately two metres per second. It was rapidly realised that this frequency corresponded to one-ninth of a day, and therefore the authenticity of this signal was in some doubt. If a non-sinusoidal oscillation is present in a time-series then power will be seen in a periodogram at not only the frequency of the oscillation, but also harmonics at integer multiples of this frequency. A re-analysis of data obtained over the period of 1974–1976 by Brookes et al.
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This is an F-type main-sequence star with a stellar classification of F0 V. Previously it had been classed as F0 III, matching an evolved giant star. It is a Delta Scuti variable, varying by an amplitude of 0.025 in B magnitude with a period of 118 minutes. At the age of 786 million years, it has a high rate of spin with a projected rotational velocity of 103 km/s. The star has 1.45 times the mass of the Sun and is radiating 12.6 times the Sun's luminosity from its photosphere at an effective temperature of 7,132 K.
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A line code (also called digital baseband modulation or digital baseband transmission method) is a code chosen for use within a communications system for baseband transmission purposes. Line coding is often used for digital data transport. Line coding consists of representing the digital signal to be transported by an amplitude- and time-discrete signal that is optimally tuned for the specific properties of the physical channel (and of the receiving equipment). The waveform pattern of voltage or current used to represent the 1s and 0s of a digital data on a transmission link is called line encoding.
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In February and March 2008, three rotational lightcurves of Vanphilos were obtained from photometric observations by astronomers Petr Pravec, James W. Brinsfield and Robert Stephens. Light-curve analysis gave a well defined rotation period of 4.225 and 4.226 hours, respectively, with a change in brightness between 0.50 and 0.54 magnitude (). In August 2014, astronomer Brian Warner derived a concurring period of 4.227 hours with an amplitude of 0.62 magnitude from his observations taken at the Palmer Divide Station in Colorado (). Light-curve plots were published on-line by the Ondřejov Observatory and the Center for Solar System Studies.
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In January 2016, the best-rated rotational lightcurve of Turnera was obtained from photometric observations by the Spanish amateur astronomer group OBAS, Observadores de Asteroids. Lightcurve analysis gave a well-defined rotation period of 12.085 hours with a brightness variation of 0.31 magnitude (). Previously, American astronomer Brian Warner obtained a similar period of 12.066 hours and an amplitude of 0.34 magnitude at his Palmer Divide Observatory () in Colorado (). Other lightcurve observations were made by French amateur astronomer Laurent Bernasconi ( hours; Δmag of 0.25; ) in February 2006, and by Italian astronomer Maria A. Barucci (12.010 hours; Δmag of 0.20; ) in August 1987.
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In May 2000, a rotational lightcurve of Jacqueline was obtained from photometric observations by American photometrist Robert Stephens at the Santana Observatory in California. Analysis of the classically shaped bimodal lightcurve gave a well-defined rotation period of hours and a brightness variation of magnitude, indicative of a non-spheroidal shape (). Other measurements by Eric Barbotin and by astronomers at the Palomar Transient Factory gave a similar period of 7.873 and 7.875 hours with an amplitude of 0.72 and 0.43 magnitude, respectively (). In 2016, a lightcurve was published using modeled photometric data from the Lowell Photometric Database.
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The Sun appears to move northward during the northern spring, contacting the celestial equator on the March equinox. Its declination reaches a maximum equal to the angle of Earth's axial tilt (23.44°) on the June solstice, then decreases until reaching its minimum (−23.44°) on the December solstice, when its value is the negative of the axial tilt. This variation produces the seasons. A line graph of the Sun's declination during a year resembles a sine wave with an amplitude of 23.44°, but one lobe of the wave is several days longer than the other, among other differences.
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In December 2000, a rotational lightcurve of Sophia was obtained from photometric observations by Bill Holliday in New Braunfels, Texas. Lightcurve analysis gave a well-defined rotation period of hours with a brightness variation of magnitude (). Between 2005 and 2013, additional observations by French amateur astronomers Laurent Bernasconi, Etienne Morelle and René Roy gave a tentative period of hours with an amplitude between 0.25 and 0.61 (). Modeled lightcurves by Josef Ďurech and Josef Hanuš, using photometric data including from the Lowell Photometric Database and from the Wide-field Infrared Survey Explorer (WISE) were published in 2018.
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Light detectors, such as photographic plates or CCDs, measure only the intensity of the light that hits them. This measurement is incomplete (even when neglecting other degrees of freedom such as polarization and angle of incidence) because a light wave has not only an amplitude (related to the intensity), but also a phase, which is systematically lost in a measurement. In diffraction or microscopy experiments, the phase part of the wave often contains valuable information on the studied specimen. The phase problem constitutes a fundamental limitation ultimately related to the nature of measurement in quantum mechanics.
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Analog television cameras scan an image as a series of horizontal lines that are stacked vertically to form a grid or "frame". The camera's progression through the frame is carefully controlled by electronic timers, known as time base generators, that produce smoothly increasing voltages. As the camera scans the image, the brightness of the location currently being scanned is also represented as a voltage. The series of varying voltages from the sensor forms an amplitude modulated (AM) signal that encodes the brightness variations along any given scan line, and spikes in the signal indicate when the line or frame changes.
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As one of the brightest stars in the sky, Arcturus has been the subject of a number of studies in the emerging field of asteroseismology. Belmonte and colleagues carried out a radial velocity (Doppler shift of spectral lines) study of the star in April and May 1988, which showed variability with a frequency of the order of a few microhertz (μHz), the highest peak corresponding to 4.3 μHz (2.7 days) with an amplitude of 60 ms−1, with a frequency separation of c. 5 μHz. They suggested that the most plausible explanation for the variability of Arcturus is stellar oscillations.
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A network of astronomers at several observatories including Raoul Behrend at Geneva Observatory, Switzerland, obtained the so-far best rated rotational light-curve of Berna. Light-curve analysis gave a rotation period of hours with a brightness variation of 0.28 magnitude (). In November 2007, photometric observations at Cerro Tololo, Chile, using its 0.9-meter Prompt5 telescope in combination with the Spitzer Space Telescope gave a concurring period of 25.46 hours with an amplitude of 0.5 magnitude (). Other light-curves were also obtained by several amateur astronomers giving a period of 6, 25.4 and 25.45 hours, respectively ().
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A rotational lightcurve of Ógyalla was obtained by the Spanish Photometric Asteroid Analysis Group (OBAS) in June 2016. Light curve analysis gave a well-defined rotation period of 17.334 hours with a brightness variation of 0.41 magnitude (). In September 2012, photometric observations at the Palomar Transient Factory gave a period of 17.2669 and 17.3038 hours with an amplitude of 0.27 and 0.25 in the R- and S-band, respectively (). The first lightcurve was already obtained in 1974, by Swedish astronomer Claes-Ingvar Lagerkvist at Uppsala Observatory from photographic photometry, but it was only fragmentary and gave a tentative period of 12 hours ().
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Pockels cells are used in a variety of scientific and technical applications. A Pockels cell, combined with a polarizer, can be used for switching between no optical rotation and 90° rotation, creating a fast shutter capable of "opening" and "closing" in nanoseconds. The same technique can be used to impress information on the beam by modulating the rotation between 0° and 90°; the exiting beam's intensity, when viewed through the polarizer, contains an amplitude-modulated signal. This modulated signal can be used for time-resolved electric field measurements when a crystal is exposed to an unknown electric field.
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In April 2007, a first rotational lightcurve of Norma was obtained from photometric observations by French amateur astronomer Pierre Antonini. Lightcurve analysis gave a rotation period of 30.6 hours with a brightness variation of 0.2 magnitude (). However more recent observations by two American astronomers have since superseded this result. In December 2011, Robert Stephens at the Santana Observatory obtained a lightcurve that gave a period 19.55 hours and a brightness amplitude of 0.06 magnitude (), while Frederick Pilcher measured a period of 19.508 hours with an amplitude of 0.25 at the Organ Mesa Observatory in November 2016.
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Petrina (minor planet designation: 482 Petrina) is a minor planet orbiting the Sun. Attempts to produce a light curve for this object have yielded differing synodic rotation periods, perhaps in part because the period is close to half an Earth day. Observations suggest that the pole of rotation is near the orbital plane, yielding only small light variations during certain parts of each orbit. Attempts to observe the asteroid photometrically during an optimal viewing period of the object's orbit gave a rotation period of 11.7922 ± 0.0001 h with an amplitude variation of 0.53 ± 0.05 in magnitude.
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In January 2012, a rotational lightcurve of Jaroslawa was obtained from photometric observations by American astronomer Maurice Clark at Preston Gott Observatory in Lubbock, Texas. Lightcurve analysis gave a long rotation period of 94.432 hours and a high brightness variation of 0.80 magnitude (). In October 2014, Frederick Pilcher at the Organ Mesa Observatory in New Mexico, in collaboration with astronomers at Etscorn and Bigmuskie observatories, obtained a refined period of 97.4 hours with an amplitude of magnitude (). This result supersedes other measurements by Maurice Clark, Nicolas Esseiva, Raoul Behrend, Laurent Bernasconi, Jean-Gabriel Bosch and Josep Coloma.
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Lightcurve-based 3D shape model of Sorga In April 2005, a rotational lightcurve of Sorga was obtained from photometric observations by Brian Warner at his Palmer Divide Observatory in Colorado. Analysis gave a classically shaped bimodal lightcurve with a well-defined rotation period of () hours and a high brightness variation of () magnitude, indicative of its elongated shape (). In February 2009, Warner revisited Sorga and determined a very similar period of () hours though with a much lower amplitude of () magnitude (). In January 2010, astronomers at the Palomar Transient Factory measured a period of hours with an amplitude of magnitude ().
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Several rotational lightcurves of Fini have been obtained from photometric observations. However, the asteroid, which shows a notably low brightness variation – indicative of a spherical rather than elongated shape – still has a poorly determined rotation period. Based on observations from February 2003 and November 2011, Brian Warner at his Palmer Divide Observatory in Colorado, determined three possible period solutions of , and hours with corresponding low amplitudes of , and magnitude (). Petr Pravec and Peter Kušnirák at Ondřejov Observatory derive a rotation period of hours from their observations in October 2001, or half of Warner's period solution, also with an amplitude of 0.2 magnitude ().
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In January 1988, a first rotational lightcurve of Nestor was obtained from photometric observations by MIT-astronomer Richard P. Binzel showing a rotation period of hours (). In August 1995, Italian astronomer Stefano Mottola observed the asteroid with the Bochum 0.61-metre Telescope at ESO's La Silla Observatory, Chile, and derived a period of hours with a brightness variation of magnitude (). In January and February 2014, two lightcurves in the R-band were obtained at the Palomar Transient Factory, California. Lightcurve analysis gave two concurring periods of and hours with an amplitude of 0.24 and 0.22, respectively ().
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This is a B-type main sequence star with a stellar classification of B1/B2 V. Sigma Lupi is a Helium strong star with an enhanced abundance nitrogen and an underabundance of carbon. Jerzykiewicz and Sterken (1992) showed a small amplitude variability with a period of 3.02 days. This suggests it is a close binary system forming a rotating ellipsoidal variable, although other causes such as rotational modulation can not be ruled out. There is a higher frequency photometric variability with a rate of 10.93482 per day and an amplitude of 0.0031 in visual magnitude, but the cause of this is unknown.
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Radial velocity measurements from High Accuracy Radial Velocity Planet Searcher with an amplitude of 4 km/s indicate that it is a spectroscopic binary of unknown period. The visible component is an A-type main-sequence star with a stellar classification of A0V, and has some slight abundance anomalies that resemble a weak Am star. It is catalogued as a shell star, showing spectral features of a cooler circumstellar jacket of gas, and may be a proto-shell star. The star is an estimated 254 million years old with a relatively low projected rotational velocity of 52 km/s.
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The pair are members of the Tucana-Horologium moving group, a 45 million year old set of stars that share a common motion through space. HD 24071 is an A-type main- sequence star with a stellar classification of A1 Va. It is a suspected variable star of unknown type showing an amplitude of 0.05 magnitude, and is a source of X-ray emission, which may originate from a companion of class G2-5V. The brighter component, HD 24072, is a B-type main-sequence star with a classification of B9.5 Van. The n suffix indicates "nebulous" absorption lines due to rapid rotation.
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A delay line interferometer (DLI) can be a Mach–Zehnder interferometer or Michelson interferometer based on two-beam interference, in which one beam is time-delayed to the other by a desired interval. Delay line interferometers are also known as optical DPSK demodulators. They convert a phase-keyed signal into an amplitude-keyed signal. In this application, an incoming differential phase-shift keying (DPSK) optical signal is first split into two equal- intensity beams in two arms of a Mach Zehnder or Michelson interferometer, in which one beam is delayed by an optical path difference corresponding to 1-bit time delay.
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This star has been catalogued with a stellar classification of B1 V:ne or B2 IVne, indicating that it is either a main sequence or a subgiant star. The 'n' indicates a nebulous spectrum created by the Doppler shift- broadened absorption lines from a rapid rotation, while the 'e' means this is a Be star, with the spectrum showing emission lines from hot, circumstellar gas. HD 153261 display some variability with an amplitude of 0.090 in magnitude, and is a suspected spectroscopic binary. HD 153261 is a large star with over ten times the Sun's mass and around 4.5 the radius of the Sun.
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Photometric observations of the asteroid by American photometrist Frederick Pilcher from his Organ Mesa Observatory in New Mexico during 2016−17 showed an irregular lightcurve with a synodic rotation period of 13.868 hours and an amplitude of 0.11 in magnitude (). This result is in good agreement with two previous observations by Robert Stephens, and by Cyril Cavadore and Pierre Antonini who measured a period of 13.82 hours and a brightness variation of 0.12 and 0.05, respectively (). Other rotational lightcurves obtained by Alan Harris (10 h; 1980), by Italian (10.47 h; 2000), and Swiss/French astronomers (13.82 h; 2005), and at the Colgate University (26.53 h; 2001), are of poor quality ().
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Lightcurve-based 3D-model of Erynia In January 2002, a rotational lightcurve of Erynia was obtained from photometric observations by French astronomer Laurent Bernasconi. Lightcurve analysis gave a rotation period of hours with a high brightness variation of magnitude, indicative of a non-spherical, elongated shape (). A concurring period of hours and an amplitude 0.47 magnitude was obtained by astronomers at the Palomar Transient Factory in April 2010 (). In 2011, a modeled lightcurve using data from the Uppsala Asteroid Photometric Catalogue (UAPC) and other sources gave a sidereal period hours, as well as two spin axes at (187.0°, −60.0°) and (335.0°, −74.0°) in ecliptic coordinates (λ, β).
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If for instance the position of one interferometer mirror vibrates and thereby causes an oscillating path length difference, the output light has an amplitude modulation of the same frequency. Independent of the existence of such a (classical) signal, a beam of light always carries at least the vacuum state uncertainty (see above). The (modulation) signal with respect to this uncertainty can be improved by using a higher light power inside the interferometer arms, since the signal increases with the light power. This is the reason (in fact the only one) why Michelson interferometers for the detection of gravitational waves use very high optical power.
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In May 2004, a rotational lightcurve of Hildrun was obtained from photometric observations by Brian Warner at the Palmer Divide Observatory in Colorado. Lightcurve analysis gave a rotation period of hours with a brightness variation of magnitude (). Two tentative lightcurves were obtained by Pierre Antonini in June 2010, and by Robin Esseiva, Nicolas Esseiva and Raoul Behrend in April 2015; both with a period of hours and an amplitude of and magnitude, respectively (). In 2016, a modeled lightcurves using photometric data from various sources, rendered a concurring sidereal period of hours and two spin axes of (247.0°, −29.0°) and (86.0°, −63.0°) in ecliptic coordinates.
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Along the southern segment, footwall bed dips define a structural high symmetrically disposed about the point of maximum throw. A prominent hanging wall feature of the southern segment is the Moab Anticline, with a crestal collapse graben accommodated by an array of normal faults. The Moab Anticline is an asymmetric fold with a wavelength of approximately 1 km, an amplitude of 350 m and a length of over 10 km. The internal geometry of the Moab fault zone is complex in terms of the numbers of slip zones, the partitioning of throw between them and the distribution of fault rocks, all of which vary over the fault surface.
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An amplitude modulation hologram is one where the amplitude of light diffracted by the hologram is proportional to the intensity of the recorded light. A straightforward example of this is photographic emulsion on a transparent substrate. The emulsion is exposed to the interference pattern, and is subsequently developed giving a transmittance which varies with the intensity of the pattern – the more light that fell on the plate at a given point, the darker the developed plate at that point. A phase hologram is made by changing either the thickness or the refractive index of the material in proportion to the intensity of the holographic interference pattern.
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Frequency Domain (FD) system comprises NIR laser sources which provide an amplitude-modulated sinusoid at frequencies near 100 MHz. FD-fNIRS measures attenuation, phase shift and the average path length of light through the tissue. Multi-Distance, which is a part of the FD-fNIRS, is insensitive to differences in skin color—giving constant results regardless of subject variation. Changes in the back-scattered signal's amplitude and phase provide a direct measurement of absorption and scattering coefficients of the tissue, thus obviating the need for information about photon path-length; and from the coefficients we determine the changes in the concentration of hemodynamic parameters.
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Several rotational lightcurves of Borodino have been obtained from photometric observations since 2007. Best-rated lightcurve by Australian amateur astronomer David Higgins at the Hunters Hill Observatory gave a rotation period of 5.442 hours with a brightness variation of 0.60 magnitude (). Other observations by French amateur astronomer Patrick Mazel, by astronomers at Texas A&M; University, using the SARA-telescopes of the Southeastern Association for Research and Astronomy consortium, and by astronomers at the Oakley Southern Sky Observatory, Australia, gave a period of 5.435, 5.437 and 5.44 hours with an amplitude of 0.74, 0.65 and 0.63 magnitude, respectively (). A high brightness amplitude is indicative of a non-spherical shape.
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Thermal emission measurements from the Wide-field Infrared Survey Explorer (WISE) gave an even higher amplitude of 1.53 magnitude. In October 2016, another lightcurve of Guinevere was obtained at the Center for Solar System Studies (CS3), Landers, in the Southern California desert, during a photometric survey conducted by American astronomers Dan Coley, Robert Stephens and Brian Warner (). It showed a period of 14.730 hours with an amplitude of 0.89 magnitude (). A 2016-published lightcurve, using modeled photometric data from the Lowell Photometric Database (LPD), gave a concurring period of 14.73081 hours (), as well as two spin axis of (19.0°, 70.0°) and (194.0°, 59.0°) in ecliptic coordinates (λ, β).
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In December 1990, a rotational lightcurve of Ennomos was obtained by Italian astronomers Stefano Mottola and Mario Di Martino using the 1.52-meter Loiano Telescope at the Observatory of Bologna in Italy. Lightcurve analysis gave a well-defined rotation period of 12.275 hours with a relatively high brightness amplitude of 0.47 magnitude (), indicative of a non-spherical, elongated shape. Between 2015 and 2017, photometric observations by Daniel Coley and Robert Stephens at the Center for Solar System Studies, California, gave several concurring periods of 12.267, 12.269 and 12.271 with an amplitude between 0.43 and 0.46 magnitude (). This also supersedes a period form Stephens taken at the GMARS Observatory in September 2011.
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In December 2002, a first rotational lightcurve of Agelaos was obtained from photometric observations over two consecutive nights by Italian astronomer Stefano Mottola with the 1.2-meter telescope at Calar Alto Observatory in Spain. Lightcurve analysis gave a rotation period of 18.61 hours with a brightness amplitude of 0.23 magnitude (). Observations in the R-band by astronomers at the Palomar Transient Factory in October 2012 gave a period of 18.456 hours with an amplitude of 0.15 magnitude (). The so-far best-rated lightcurve by Robert Stephens at the Center for Solar System Studies in Landers, California, gave a concurring period of and a brightness variation of 0.19 ().
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According to the surveys carried out by PanSTARRS, Kiuchi is a bright V-type asteroid. The Collaborative Asteroid Lightcurve Link assumes an albedo of 0.40 and calculates a diameter of 3.86 kilometers, using an absolute magnitude of 13.676 from Petr Pravec's revised WISE data. Kiuchi itself has a rotation period of hours with a small brightness variation of 0.1 magnitude, indicating a nearly spheroidal shape (). Photometric follow-up observations by Petr Pravec confirmed the results in 2013 and 2016, giving a period of 3.6198 and 3.6196 hours with an amplitude of 0.08 and 0.1 magnitude, and an orbital period for the satellite of 20.9 and 20.9062 hours, respectively ().
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Despite its enlarged girth, this star is still spinning with a slightly faster equatorial azimuthal velocity than the Sun, having a projected rotational velocity of 3.44 km s−1. Hamal is radiating about 91 times the Sun's luminosity from its outer envelope at an effective temperature of 4,480 K. This is cooler than the surface of the Sun, giving it the orange-hued glow of a K-type star. It is suspected to be slightly variable, with an amplitude of 0.06 magnitude. The abundance of elements other than hydrogen and helium, what astronomers term the star's metallicity, is only around half that in the Sun.
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Hygiea has a rotation period of about 13.8256 hours, determined from observations with the VLT in 2017 and 2018. Its single-peaked light curve has an amplitude of 0.27 mag, which is largely attributed to albedo variations. , the direction of Hygiea's rotation is not known, due to a twofold ambiguity in lightcurve data that is exacerbated by its long rotation period—which makes single-night telescope observations span at best only a fraction of a full rotation—but it is believed to be retrograde. Lightcurve analysis indicates that Hygiea's pole points towards either ecliptic coordinates (β, λ) = (30°, 115°) or (30°, 300°) with a 10° uncertainty.
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2 Vulpeculae is a binary star system in the northern constellation of Vulpecula, located around 1,800 light years away from the Sun. It is visible to the naked eye as a faint, blue-white hued star with an apparent visual magnitude of 5.43. 2 Vulpeculae is a double-lined spectroscopic binary; as of 2002, the pair had an angular separation of along a position angle of 127.2°. The primary component of the binary is a rapidly rotating Be star with a stellar classification of B1 IV. It is a variable star with an amplitude of 0.06 magnitude and a period of 0.6096 days, tentatively classified as Beta Cephei variable.
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70-400 kHz, and with an amplitude of 20-100 nm, high enough to allow the tip to not get stuck to the sample because of the adhesion force. The atomic force microscope can be used as a nanoindenter in order to measure hardness and Young's modulus of the sample. For this application, the tip is made of diamond and it is pressed against the surface for about two seconds, then the procedure is repeated with different loads. The hardness is obtained dividing the maximum load by the residual imprint of the indenter, which can be different from the indenter section because of sink-in or pile-up phenomena.
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The eccentricity of its orbit allows it to alternately pass inside and outside of Jupiter's orbit at its closest approaches of 176 million kilometers. Each time it passes near Jupiter its orbital elements, including its period, are slightly altered. Over thousands of years the angle between the position of the asteroid and its perihelion minus the angle between Jupiter and the asteroid's perihelion tends to oscillate around zero with a period of about 660 years and an amplitude of about 125°, although sometimes this difference slips by a whole 360°. The adjunct diagram shows one complete orbit of asteroid Kaʻepaokaʻawela in a frame of reference rotating with Jupiter.
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Astronomers Maryanne Angliongto and Milan Mijic at Cal State LA, United States, obtained a rotational lightcurve of Srbija in May 2006. It gave a rotation period of 29.64 hours with a brightness variation of 0.37 magnitude (). In November 2009, photometric observations by James W. Brinsfield at Via Capote Observatory , California, gave a shorter period of 9.135 hours with an amplitude of 0.17 (). According to the space-based surveys carried out by the Japanese Akari satellite and NASA's Wide-field Infrared Survey Explorer with its subsequent NEOWISE mission, Srbija measures between 29.48 and 43.23 kilometers in diameter, and its surface has an albedo between 0.042 and 0.10.
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In 2009 and 2010, two fragmentary lightcurves of ' were obtained from photometric observations by Stefano Mottola at the Calar Alto Observatory in Spain. Lightcurve analysis gave a tentative rotation period of 13.696 and 13.70 hours with a brightness variation of 0.14 and 0.06 magnitude, respectively (). During 2015–2017, three additional photometric observation were made at the Californian Center for Solar System Studies by Robert Stephens, Daniel Coley and Brian Warner in collaboration with Linda French from Illinois Wesleyan University. The two best-rated lightcurves gave a period of 17.383 and 17.44 with an amplitude of 0.08 and 0.11 magnitude, respectively, indicating that the body has a nearly spherical shape ().
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Features include four voltage-controlled oscillators (VCOs) with tuning, footage (16, 8, 4, 2), waveshape (triangle, saw, pulse-width, and pulse-width modulated), and amplitude. The first oscillator is the master oscillator as far as fine tuning goes. Two direct modifiers to the VCOs are a detune control that only affects oscillators 2 and 4, and a Pulse Width control that goes to cancellation either side of 50% phase symmetry of a square wave; pulse width can be routed to MG1, MG2, or voltage-controlled filter (VCF) envelope. There is one independent noise generator with an amplitude control (frequency and shape is modified by the VCF).
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In March 2009, a rotational lightcurve of Merope was obtained from photometric observations by astronomers at the Oakley Southern Sky Observatory in Australia. Lightcurve analysis gave a rotation period of 27.2 hours with a brightness variation of 0.20 magnitude (). In October 2012, astronomers at the Palomar Transient Factory in California measured a period 13.717 hours with an amplitude of 0.11 magnitude in the R-band (), which seems to be an alternative period solution (1:2 alias) of what the Australian astronomers had previously measured. Previous observations by Gino Farroni and by Federico Manzini from 2004 and 2005, respectively, have been provisional and of poor quality ().
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This indicates the star has reached a stage in its evolution where it has expanded to become a supergiant with 169 times the radius of the Sun. As this is a massive star with 8–13 times the mass of the Sun, it rapidly burns through its supply of nuclear fuel and has become a supergiant in roughly , after spending as a main sequence star. l Carinae is classified as a Cepheid variable star and its brightness varies over an amplitude range of 0.725 in magnitude with a long period of 35.560 days. The radial velocity of the star likewise varies by 39 km/s during each pulsation cycle.
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This object is an evolved K-type giant star with a stellar classification of , where the suffix notation indicates this is an intermediate CN star. It is a periodic microvariable with an amplitude of 0.0055 magnitude and a frequency of 0.36118 cycles per day. With the supply of hydrogen exhausted at its core, the star has expanded and cooled, now having 31 times the Sun's girth. It is radiating 338.5 times the luminosity of the Sun from its swollen photosphere at an effective temperature of 4,420 K. Eta Gruis has a magnitude 11.5 visual companion located at an angular separation of along a position angle of 187°, as of 2012.
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In May 2002, a rotational lightcurve of Zulu was obtained from photometric observations by American astronomer Robert Stephens at the Santana Observatory in California. Lightcurve analysis gave a well-defined rotation period of 18.64 hours with a brightness variation of 0.11 magnitude (). One month later, French amateur astronomers René Roy and Laurent Brunetto obtained another lightcurve with a concurring period of 18.65 hours and an amplitude of 0.09 magnitude (). According to the survey carried out by NASA's Wide-field Infrared Survey Explorer with its subsequent NEOWISE mission, Zulu measures 12.41 and 20.561 kilometers in diameter and its surface has an albedo of 0.055 and 0.16.
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In September 1994, photometric observations of Ulysses were made by astronomers Stefano Mottola and Uri Carsenty at ESO's La Silla Observatory, Chile, using the Bochum 0.61-metre Telescope. The observations were used to build a lightcurve showing a well- defined rotation period of 28.72 hours with a brightness variation of 0.32 magnitude (). In March 2014, another rotational lightcurve was obtained in the R-band by astronomers at the Palomar Transient Factory, California, which gave a concurring period of 28.7840 hours with an amplitude of 0.33 magnitude (). While not being a slow rotator, Ulysses period longer than the 2 to 20 hours measured for most asteroids.
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In conventional black and white (B&W;) televisions, the CRT screen has a uniform coating of phosphor that emits white light when struck by electrons. The beam from an electron gun at the back of the tube is deflected (most commonly) by the varying fields from magnetic coils so it may be directed at any point on the screen. Electronic circuits known as time base generators pull the beam across the tube and down, creating the scanning pattern used in television signals. An amplitude modulated signal is used to control the acceleration of the beam, controlling the brightness as it is pulled across the screen.
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Reflected ultrasound comes from an interface, such as the back wall of the object or from an imperfection within the object. The diagnostic machine displays these results in the form of a signal with an amplitude representing the intensity of the reflection and the distance, representing the arrival time of the reflection. In attenuation (or through- transmission) mode, a transmitter sends ultrasound through one surface, and a separate receiver detects the amount that has reached it on another surface after traveling through the medium. Imperfections or other conditions in the space between the transmitter and receiver reduce the amount of sound transmitted, thus revealing their presence.
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In May 2005, a rotational lightcurve of Henry was obtained by French amateur astronomer Christophe Demeautis. It gave a rotation period of 17.370 hours with a brightness variation of 0.54 magnitude (). In February 2010, photometric observations by David Polishook and others at the Californian Palomar Transient Factory gave a divergent period of 10 hours with an amplitude of only 0.04 (). According to the surveys carried out by the Infrared Astronomical Satellite IRAS, the Japanese Akari satellite, and NASA's Wide-field Infrared Survey Explorer with its subsequent NEOWISE mission, Henry measures between 19.19 and 28.55 kilometers in diameter, and its surface has an albedo between 0.039 and 0.070.
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Photometric observations of this asteroid at the Oakley Observatory in Terre Haute, Indiana, during 2006 gave a light curve with a period of 11.13 ± 0.02 hours and a brightness variation of 0.55 ± 0.02 in magnitude (). A better rated lightcurve, already obtained by Alan Harris in October 1979, gave a period of 11.173 hours with an amplitude of 0.35 (). A modeled lightcurve using photometric data from a larger international collaboration was published in 2016. It gave a period of 11.17342 hours, identical to the 1979-observations by Harris, as well as two spin axes at (65.0°, −6.0°) and (248.0°, −9.0°) in ecliptic coordinates (λ, β).
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In October 2006, ground-based photometric observations were used in an attempt to measure Annefranks rotational period. Analysis of the ambiguous lightcurve gave a period of hours and a brightness variation of 0.25 magnitude with two alternative period solutions of 12 and 22.8 hours, respectively (). In January 2014, photometric observations at the Palomar Transient Factory gave a rotation period of and hours with an amplitude of 0.17 and 0.20 magnitude, respectively (). The lightcurve data suggests that Annefrank is not Lambertian, meaning that surface features, such as shadows from boulders and craters, play a role in the object's perceived brightness and not just the asteroid's relative size when seen from that orientation.
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The primary, component Aa, is a Be star that is surrounded by ionized gas that is producing the emission lines in the spectrum. This circumstellar shell is inclined by 80° to the line of sight from the Earth. The system is undergoing both short term and long term variations in luminosity, with the short period variations showing a phase cycle of 1.03 days. It is classified as a Gamma Cassiopeiae variable with an amplitude of 0.16 in magnitude. Epsilon Capricorni Aa is a blue-white hued B-type main sequence star with a stellar classification of B2.5 Vpe and a visual magnitude of +4.62.
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Symbiotic novae are slow irregular eruptive variable stars with very slow nova-like outbursts with an amplitude of between 9 and 11 magnitudes. The symbiotic nova remains at maximum for one or a few decades, and then declines towards its original luminosity. Variables of this type are double star systems with one red giant, which probably is a Mira variable, and one white dwarf, with markedly contrasting spectra and whose proximity and mass characteristics indicate it as a symbiotic star. The red giant fills its Roche lobe so that matter is transferred to the white dwarf and accumulates until a nova-like outburst occurs, caused by ignition of thermonuclear fusion.
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In June 2015, a rotational lightcurve of Purple Mountain was obtained from photometric observations by astronomers at Texas A&M; University, using the SARA-telescopes of the Southeastern Association for Research and Astronomy consortium. The 0.9-meter SARA-North telescope is located at Kitt Peak National Observatory, Arizona, while the 0.6-meter SARA-South telescope is hosted at the Cerro Tololo Inter-American Observatory in Chile. Lightcurve analysis gave a rotation period of 5.857 hours with a brightness variation of 0.32 magnitude (). One month later, in July 2015, another period of 2.928 hours and an amplitude of 0.40 magnitude was measured at MIT's George R. Wallace Jr. Observatory ().
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The former hosts the government office where every visitor has to pay a tax. The latter is used as the port for the tourist boats arriving from the mainland and has several souvenir shops selling items like coral and shells and plastic-encased butterflies, scorpions, and spiders. Beaches and caves are regularly flooded with the tides, which have an amplitude of , so access to some caves is only possible during low tide. The Thai name for Khao Phing Kan reflects the particular shape of the island which appears as if a flat limestone cliff tumbled sideways and leaned on a similar rock in the centre of the island.
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One 9-year study of temperature, granulation, and the chromosphere showed no systematic variations; Ca II emissions around the H and K infrared bands show a possible 11-year cycle, but this is weak relative to the Sun. Alternatively it has been suggested that the star could be in a low-activity state analogous to a Maunder minimum—a historical period, associated with the Little Ice Age in Europe, when sunspots became exceedingly rare on the Sun's surface. Spectral line profiles of Tau Ceti are extremely narrow, indicating low turbulence and observed rotation. The star's oscillations have an amplitude about half that of the Sun and a lower mode lifetime.
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It is a Delta Scuti variable with a period of 0.1327 days and an amplitude of 0.050 magnitude. With an estimated age of 1.168 billion years, it is spinning rapidly with a projected rotational velocity of 124.2 km/s and a rotation period of 1.2 days. The star has about 1.57 times the mass of the Sun and 2.79 times the Sun's radius. (De Rosa and colleagues give a mass estimate of 2.20 times the Sun's mass.) It is radiating around 29.5 times the solar luminosity from its outer atmosphere at an effective temperature of 7,211 K. The companion, component B, is a magnitude +11.0 star.
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In October 1998, a rotational lightcurve of Thüringia was obtained from photometric observations by astronomers of the Minnesota State University Moorhead at Paul Feder Observatory. Analysis of the classically shaped bimodal lightcurve gave a well-defined rotation period of hours with a high brightness variation of magnitude, indicative of an irregular, non-spherical shape (). In October 2007, another period determination by Federico Manzini, Hiromi Hamanowa and Hiroko Hamanowa determined a period of hours and an amplitude of magnitude (). In 2011, a modeled lightcurve using data from the Uppsala Asteroid Photometric Catalogue (UAPC) and other sources gave a sidereal period 8.16534 hours, as well as a spin axis of (120.0°, −52.0°) in ecliptic coordinates (λ, β) ().
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At these extreme points this effect varies the apparent solar day by 7.9 s/day from its mean. Consequently, the smaller daily differences on other days in speed are cumulative until these points, reflecting how the planet accelerates and decelerates compared to the mean. As a result, the eccentricity of the Earth's orbit contributes a periodic variation which is (in the first-order approximation) a sine wave with an amplitude of 7.66 min and a period of one year to the equation of time. The zero points are reached at perihelion (at the beginning of January) and aphelion (beginning of July); the extreme values are in early April (negative) and early October (positive).
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2013, work in progress # A low mass binary: One of the binary system observed by CoRoT is of particular interest since the less massive component is a late M star of 0.23 M⊙ with an estimated effective temperature of about 3000 K.Gandolfi, D. et al. 2013, work in progress The primary component is a 1.5 M⊙ star MS star. # A beaming effect in a binary: A binary system observed by CoRoT showed out of eclipses variations which were interpreted as a beaming effect (also called Doppler boosting). This effect results from the variation in brightness of source approaching or moving away from the observer, with an amplitude proportional to the radial velocity divided by the speed of light.
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Lightcurve-based 3D-model of Banachiewicza In August 2008, the best-rated rotational lightcurve of Banachiewicza was obtained from photometric observations by French amateur astronomers Laurent Bernasconi, Cyril Cavadore and Stéphane Charbonnel. Lightcurve analysis gave a rotation period of 8.631 hours with a brightness variation of 0.54 magnitude, indicative for an irregular, elongated shape (). Other observations at the Palomar Transient Factory in California, and by a collaboration of Hungarian astronomers gave a period of 8.628 and 5 hours with an amplitude of 0.36 and 0.4 magnitude, respectively (). In 2013, an international study modeled a lightcurve with a concurring period of hours and found two spin axis of (214.0°, 62.0°) and (64.0°, 60.0°) in ecliptic coordinates (λ, β) ().
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An HP 8590L (low cost version of 8591c), video out connected to a Cadco channel modulator operating above 550 MHz, with a Radio Shack black and white TV (picture tube) tuned to UHF channels to see the picture. Add to that a comb generator with 4-6 CW tones, an HP Calan 1776 "portable" spectrum analyzer.. Not all amplifiers contained a good return path test point, so the repair lab was asked to modify some line extender diplex filters to pass the forward, and divert the return path to an F connector. A pad socket was also converted. Any signal entering an amplifier with an amplitude above -45 dBmV was located and fixed.
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A variation in surface temperature induced by climate changes and the Milankovitch cycle can penetrate below the Earth's surface and produce an oscillation in the geothermal gradient with periods varying from daily to tens of thousands of years and an amplitude which decreases with depth and having a scale depth of several kilometers. pp. 183-4 pp. 187-9 Melt water from the polar ice caps flowing along ocean bottoms tends to maintain a constant geothermal gradient throughout the Earth's surface. If the rate of temperature increase with depth observed in shallow boreholes were to persist at greater depths, temperatures deep within the Earth would soon reach the point where rocks would melt.
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In September 2007, a rotational lightcurve of Jürgenstock was obtained from photometric observations by Federico Manzini at the Sozzago Astronomical Station in Italy. Lightcurve analysis gave a rotation period of hours with a brightness variation of 0.11 magnitude, indicative of a spherical rather than elongated shape (). In July 2014, a similar period determination of hours and an amplitude of 0.10 magnitude was made by Brian Warner at the Palmer Divide Station in California (). While Manzini and/or Raoul Behrend suspected it to be an asynchronous binary asteroid with a minor-planet moon in its orbit, Warner did not mention any anomalies in the lightcurve, and the Lightcurve Data Base does not flag the body as a potential binary system.
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Artist's impression of Varuna depicting its reddish color and ellipsoidal shape Varuna has a rapid rotation period of approximately 6.34 hours, derived from a double-peaked solution for Varuna's rotational light curve. Varuna's rotation was first measured January 2001 by astronomer Tony Farnham using the McDonald Observatory's 2.1-meter telescope, as part of a study on the rotation and colors of distant objects. CCD photometry of Varuna's light curve in 2001 revealed that it displays large brightness variations with an amplitude of about 0.5 magnitudes. The measured rotational light curve of Varuna provided two ambiguous rotation periods of 3.17 and 6.34 hours, for a single-peaked and a double-peaked solution, respectively.
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The Watson-Watt technique uses two Adcock antenna pairs to perform an amplitude comparison on the incoming signal. An Adcock antenna pair is a pair of monopole or dipole antennas that takes the vector difference of the received signal at each antenna so that there is only one output from the pair of antennas. Two of these pairs are co- located but perpendicularly oriented to produce what can be referred to as the N-S (North-South) and E-W (East-West) signals that will then be passed to the receiver. In the receiver, the bearing angle can then be computed by taking the arctangent of the ratio of the N-S to E-W signal.
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Although their short-term photometric data was insufficient for Ixion's rotation period to be determined based on its brightness variations, they were able to constrain Ixion's light curve amplitude below 0.15 magnitudes. Astronomers Sheppard and Jewitt obtained similarly inconclusive results in 2003 and provided an amplitude constraint less than 0.05 magnitudes, considerably less than Ortiz's amplitude constraint. In 2010, astronomers Rousselot and Petit observed Ixion with the European Southern Observatory's New Technology Telescope and determined Ixion's rotation period to be hours, with a light curve amplitude around 0.06 magnitudes. Galiazzo and colleagues obtained a shorter rotation period of hours in 2016, though they calculated that there is a 1.2% probability that their result may be erroneous.
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Then: > From our perspective on Earth, this would appear as a displacement, or > polarization, of the lunar orbit away from the Sun with an amplitude of 13 > meters. If the violation went the other way, with the self energy possessing > inertial mass but not gravitational mass, the lunar orbit would appear to be > polarized toward the Sun by the same amplitude. The calculation of the > amplitude is complicated, but a crude estimate may be derived by multiplying > the Earth’s orbital radius of by the contribution to the Earth’s mass from > the self-energy to yield 75 meters. The signature of an EP violation is very simple, depending only on the distance of the Moon from the Sun.
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In statistics, signal processing, and time series analysis, a sinusoidal model to approximate a sequence Yi is: :Y_i = C + \alpha\sin(\omega T_i + \phi) + E_i where C is constant defining a mean level, α is an amplitude for the sine wave, ω is the frequency, Ti is a time variable, φ is the phase, and Ei is the error sequence in approximating the sequence Yi by the model. This sinusoidal model can be fit using nonlinear least squares; to obtain a good fit, nonlinear least squares routines may require good starting values for the constant, the amplitude, and the frequency. Fitting a model with a single sinusoid is a special case of least-squares spectral analysis.
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The heterodyne color- under process of U-Matic, Betamax & VHS lent itself to minor modification of VCR players to accommodate NTSC format cassettes. The color-under format of VHS uses a 629 kHz subcarrier while U-Matic & Betamax use a 688 kHz subcarrier to carry an amplitude modulated chroma signal for both NTSC and PAL formats. Since the VCR was ready to play the color portion of the NTSC recording using PAL color mode, the PAL scanner and capstan speeds had to be adjusted from PAL's 50 Hz field rate to NTSC's 59.94 Hz field rate, and faster linear tape speed. The changes to the PAL VCR are minor thanks to the existing VCR recording formats.
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A three-dimensional model of 732 Tjilaki based on its light curve In February 1996, a rotational lightcurve of Tjilaki was obtained from photometric observations over ten nights by European astronomers using the Dutch 0.9-metre Telescope and the Bochum 0.61-metre Telescope at La Silla Observatory in Chile. Lightcurve analysis gave a rotation period of hours with a brightness variation of magnitude (). In May 2012, astronomers at the Palomar Transient Factory measured a period of hours (). Additional observations were made by the TESS-team in January 2019, and by amateur astronomers Axel Martin and Rui Goncalves in May 2020, reporting a concurring period of () and () hours with an amplitude of () and () magnitude, respectively ().
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Near-periodic waves over shallow water The concept of wavelength is most often applied to sinusoidal, or nearly sinusoidal, waves, because in a linear system the sinusoid is the unique shape that propagates with no shape change – just a phase change and potentially an amplitude change. See The wavelength (or alternatively wavenumber or wave vector) is a characterization of the wave in space, that is functionally related to its frequency, as constrained by the physics of the system. Sinusoids are the simplest traveling wave solutions, and more complex solutions can be built up by superposition. In the special case of dispersion- free and uniform media, waves other than sinusoids propagate with unchanging shape and constant velocity.
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The stellar classification of this star, G4 II–III, places it midway between the giant and bright giant stages of its evolution. The interferometry-measured angular diameter of this star is about 2.42 mas, which, at its estimated distance, equates to a physical radius of about 14 times the radius of the Sun. It has about three times the mass of the Sun and radiates 138 times the Sun's luminosity from its outer atmosphere at an effective temperature of 5,282 K, giving it the yellowish hue of a G-type star. In 1963, East German astronomer Gerhard Jakisch reported this star as a variable with a period of 358 days and an amplitude of 0.08 magnitude.
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Like in Alpha² Canum Venaticorum variable stars, CG Andromedae shows a variation of luminosity and one in the strength of spectral lines with the same period of approximately 3.74 days. It is thought that this is caused by an inhomogeneous distribution of elements on the surface of the star, which cause an inhomogeneous surface brightness. A shorter period, slightly longer than 2 hours, with an amplitude of 0.011 magnitudes has been observed in the light curve of CG Andromedae; however, with a temperature of 11,000 K, it lies outside the instability strip of the HR diagram where rapidly oscillating Ap stars are located. Magnetohydrodynamic waves propagating in the star could explain the observed variability.
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The long and narrow rectangular shape of the Adriatic Sea is the source of an oscillating water motion (called seiche) along the basin's minor axis.Introduction to Previsioni di Marea nell'Alto Adriatico (in Italian), Venice, issue 29 of year 29, by Stefano Fracon The principal oscillation, which has a period of 21 hours and 30 minutes and an amplitude around 0.5 meters at the axis' extremities, supplements the natural tidal cycle, so that the Adriatic Sea has much more extreme tidal events than the rest of the Mediterranean. A secondary oscillation is also present, with an average period of 12 hours and 11 minutes.Stravisi, Franco: Caratteristiche meteorologiche e climatiche del Golfo di Trieste , Università degli Studi di Trieste, Dipartimento di Scienze della Terra.
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The first significant detection of a non-transiting planet using transit-timing variations was carried out with NASA's Kepler telescope. The transiting planet Kepler-19b shows transit-timing variation with an amplitude of 5 minutes and a period of about 300 days, indicating the presence of a second planet, Kepler-19c, which has a period that is a near-rational multiple of the period of the transiting planet. In 2010, researchers proposed a second planet orbiting WASP-3 based on transit-timing variation,Planet found tugging on transits , Astronomy Now, 9 July 2010 but this proposal was debunked in 2012. Transit-timing variation was first convincingly detected for planets Kepler-9b and Kepler-9c and gained popularity by 2012 for confirming exoplanet discoveries.
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In July 2007, French amateur astronomer René Roy obtained a rotational lightcurve from photometric observations, giving a rotation period of 16 hours with a brightness variation of 0.6 magnitude (). In March 2010, photometric observations at the Palomar Transient Factory gave a shorter period of 11.843 hours with an amplitude of 0.35 magnitude (). According to the space-based survey carried out by the Japanese Akari satellite and NASA's Wide-field Infrared Survey Explorer with its subsequent NEOWISE mission, La Silla measures 12.32 and 12.96 kilometers in diameter, and its surface has an albedo of 0.054 and 0.08, respectively. The Collaborative Asteroid Lightcurve Link assumes an albedo of 0.21 – derived from 15 Eunomia, the family's largest member and namesake – and calculates a diameter of 6.64 kilometers.
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In December 2009 and June 2016, rotational lightcurves of Antilochus were obtained from photometric observations by American astronomer Robert Stephens at the Santana Observatory and at the Center for Solar System Studies (CS3) in California. Lightcurve analysis gave a rotation period of 31.52 and 31.54 hours with an amplitude of 0.09 and 0.11 magnitude, respectively (). Follow-up observations over a total of 11 nights by Stephens in August 2017 gave the so-far best-rated lightcurve with a period of hours – which corresponds to half the period solution of the former results – and a slightly higher brightness variation of 0.12 magnitude (). Stephen's period determination supersedes previously reported results by Vincenzo Zappalà (1985; 12 h), Federico Manzini (2007; 12 h) and René Roy (2009; 22.5 h) ().
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Between 1999 and 2014, several rotational lightcurves of Vyssotsky were obtained by American astronomer Brian D. Warner at his Palmer Divide Observatory, Colorado (see video in ). Light-curve analysis gave a concurring rotation period of 3.201 hours with an averaged brightness variation of 0.18 magnitude (). Additional well-defined lightcurves were obtained by astronomers Domenico Licchelli in November 2005 (), Raymond Poncy, Raoul Behrend, René Roy, Reiner Stoss, Jaime Nomen, Salvador Sanchez also in November 2005 (), David Higgins in May 2007 (), Michael Lucas in November 2010 (), as well as by Hiromi Hamanowa and Hiroko Hamanowa also in November 2010 (). The most recent photometric observation was made by Robert D. Stephens in September 2015, giving a period of 3.204 hours with an amplitude of 0.24 magnitude ().
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The Acoustisizer is an electroacoustic musical instrument built from a small grand piano with built-in speakers, magnetic guitar pickups, PZMs, and prepared piano strings. It was built as part of a graduate thesis project at California State University Dominguez Hills by Bob Fenger (1983), a student of Richard Bunger (author of the Well Prepared Piano). Speakers are built into the bottom of the instrument, redirecting its own amplified sound back onto the sounding board, with strings and magnetic pickups creating an amplitude intensity loop, which in turn drives and vibrates suspended kinetic oscillators (assemblages of vibration sensitive materials). Secondary control parameters allow extraction of vibration and sound phenomena from the kinetic oscillators through a series of proximity microphones and PZMs (piezo-electric contact mics).
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In June 2006, a rotational lightcurve of was obtained from photometric observation taken by American astronomer Brian Warner at his Palmer Divide Observatory in Colorado. Lightcurve analysis gave a rotation period of 47 hours with a brightness variation of 0.35 magnitude (), superseding a lightcurve previously obtained by Czech astronomer Petr Pravec at Ondřejov Observatory in 2003, which gave a shorter period of 29 hours and an amplitude of 0.3 magnitude (). According to the survey carried out by the Japanese Akari satellite, the asteroid measures 1.12 kilometers in diameter and its surface has an albedo of 0.428, while the Collaborative Asteroid Lightcurve Link assumes an albedo of 0.040 and calculates a diameter of 3.49 kilometers with an absolute magnitude of 16.4.
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Jones studied Electronic Engineering at the University of Liverpool, and has used his electronics skills to potent effect over the years. In the late 1970s, he designed and built various analog signal processors for use with the bass, perhaps the most unusual of which was an amplitude- and frequency-sensitive flanger that would vary the character of its flanging effect based on what notes were being played into it, and how loudly they were being played. His other designs included an envelope- controlled Voltage Controlled Filter (VCF), which can be heard on the track "Noddy Goes to Sweden" on Brand X's 1980 album Do They Hurt?, as well as an analog drum machine, which featured preset rhythms in various odd time signatures such as 15/16.
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The neper is the change in the level of a field quantity when the field quantity changes by a factor of e, that is , thereby relating all of the units as nondimensional natural log of field-quantity ratios, . Finally, the level of a quantity is the logarithm of the ratio of the value of that quantity to a reference value of the same kind of quantity. Therefore, the bel represents the logarithm of a ratio between two power quantities of 10:1, or the logarithm of a ratio between two field quantities of :1. Two signals whose levels differ by one decibel have a power ratio of 101/10, which is approximately 1.25893, and an amplitude (field quantity) ratio of 10 (1.12202).
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This frequency was chosen to minimize the chrominance beat interference pattern that would be visible in areas of high color saturation in the transmitted picture. At certain times, the chrominance signal represents only the U signal, and 70 nanoseconds (NTSC) later, the chrominance signal represents only the V signal. (This is the nature of the quadrature amplitude modulation process that created the chrominance signal.) About 70 nanoseconds later still, -U, and another 70 nanoseconds, -V. So to extract U, a synchronous demodulator is utilized, which uses the subcarrier to briefly gate (sample) the chroma every 280 nanoseconds, so that the output is only a train of discrete pulses, each having an amplitude that is the same as the original U signal at the corresponding time.
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In May 2018, a rotational lightcurve of Ani was obtained from photometric observations by American amateur astronomer Tom Polakis at the Command Module Observatory in Arizona . Lightcurve analysis gave a well-defined rotation period of hours with a brightness variation of magnitude (). In June 2002, Brian Warner at his Palmer Divide Observatory first observed this asteroid and later derived a period of hours and an amplitude of magnitude, based on poor data (). In December 2004, and in May 2007, two periods of and with a corresponding amplitude of and magnitude were determined by European astronomers Raymond Poncy as well as Yves Revaz, Raoul Behrend, Alain Klotz, Michel Hernandez, Robert Soubie, Jean-François Gauthier, Bernard Tregon, Pierre Antonini, Laurent Bernasconi, Federico Manzini , Yassine Damerdji and Horacio Correia.
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This happens as follows: Due to CP-symmetry violating electroweak interactions, some amplitudes involving quarks are not equal to the corresponding amplitudes involving anti-quarks, but rather have opposite phase (see CKM matrix and Kaon); since time reversal takes an amplitude to its complex conjugate, CPT-symmetry is conserved. Though some of their amplitudes have opposite phases, both quarks and anti-quarks have positive energy, and hence acquire the same phase as they move in space-time. This phase also depends on their mass, which is identical but depends both on flavor and on the Higgs VEV which changes along the domain wall. Thus certain sums of amplitudes for quarks have different absolute values compared to those of anti-quarks.
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While everyday wind waves have a wavelength (from crest to crest) of about and a height of roughly , a tsunami in the deep ocean has a much larger wavelength of up to . Such a wave travels at well over , but owing to the enormous wavelength the wave oscillation at any given point takes 20 or 30 minutes to complete a cycle and has an amplitude of only about .Earthsci.org, Tsunamis This makes tsunamis difficult to detect over deep water, where ships are unable to feel their passage. The velocity of a tsunami can be calculated by obtaining the square root of the depth of the water in metres multiplied by the acceleration due to gravity (approximated to 10 m/s2).
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The device that did this was called a "detector". The detector used in receivers of that day, called a coherer, simply acted as a switch, that conducted current in the presence of radio waves, and thus did not have the capability to demodulate, or extract the audio signal from, an amplitude modulated radio wave. The simplest way to extract the sound waveform from an AM signal is to rectify it; remove the oscillations on one side of the wave, converting it from an alternating current to a varying direct current. The variations in the amplitude of the radio wave that represent the sound waveform will cause variations in the current, and thus can be converted to sound by an earphone.
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The Crosby system was an FM stereophonic broadcasting standard developed by Murray G. Crosby. In the United States, it competed with, and ultimately lost to, the Zenith/GE system, which the FCC chose as the standard in 1961. While both systems used multiplexing to transmit the L-R stereo signal, the Crosby system used a frequency-modulated 50 kHz subcarrier, whereas the competing Zenith/GE system used an amplitude-modulated 38 kHz subcarrier. As FM is less susceptible to interference and noise than AM, the Crosby system had better frequency response and less noise of the two systems especially under weak signal conditions. However, the Crosby system was incompatible with existing subsidiary communications authorization (SCA) services which used subcarrier frequencies including 41 and 67 kHz.
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Last judgement. Mixed media on canvas, 40 x 50 cm, 2017 From 2015 on, Froehlich has gradually begun to change his focus from crowds to the human being in all their various individualities, with the Renaissance as his gateway to the subject, having concentrated mainly on sketching over a period of two years. The artist has, for example, used a pre-existing drawing or art work which he has magnified, while often focussing on amplifying a specific detail . This has given his compositions an amplitude and a liberty which bring them into line with the spirit of our times, using a multitude of techniques: pencil, charcoal, water colour, collage, acrylics and even encaustic painting, a very ancient technique using beeswax.
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The AN-FPQ 6 radar was built by RCA and was, effectively, a development of the AN-FPS 16. The Q6, as it was known by those who worked on it, was an amplitude comparison monopulse C-band radar, with a 2.8 MW peak klystron transmitter tunable from 5.4 to 5.8 GHz, which had a 9-meter parabolic antenna, having 52 dB gain, a 0.6 degree beam width, utilizing a Cassegrainian feed with a five horn monopulse comparator. This radar had an unambiguous maximum range of 215 or , and employed uncooled parametric amplifiers with a system noise temperature of 440 K, [a noise figure of 4 dB]. A major features of the radar was its maximum unambiguous range of despite a pulse repetition frequency [PRF]of some hundreds of pulses per second.
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Lightcurve-based 3D-model of Rotraut Two rotational lightcurves of Rotraut were obtained from photometric observations by Richard Ditteon at Oakley Southern Sky Observatory , Australia, in February 2017, and by Tom Polakis at the Command Module Observatory in Arizona in May 2018. Lightcurve analysis gave an identical rotation period of hours with a brightness variation of and magnitude, respectively (). The result supersedes a tentative period determination of hours and an amplitude of magnitude by French amateur astronomers Stéphane Charbonnel and Claudine Rinner from July 2002 (). In 2016, a modeled lightcurve gave a sidereal period of hours using data from the Uppsala Asteroid Photometric Catalogue, the Palomar Transient Factory survey, and individual observers (such as above), as well as sparse-in-time photometry from the NOFS, the Catalina Sky Survey, and the La Palma surveys .
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A large number of rotational lightcurves of Mentor have been obtained, since its first photometric observations by William Hartmann (1988). The first rotation period of hours with a brightness variation of was reported by Stefano Mottola, who observed Mentor in February 1993, using the former ESO 1-metre telescope at the La Silla Observatory in Chile (). Follow-up observations by Mottola at the Calar Alto Observatory in July 1998 gave a refined period of hours and an amplitude of magnitude (). In 2006 and 2007, photometric observations of Mentor were made at the Roque de los Muchachos (7.68 and 7.682 h) and Oakley Observatory (7.70 h). Additional period determinations by Laurent Bernasconi (7.699 h) Federico Manzini (>6 h) and René Roy (7.727 and 7.6 h) were made between 2006 and 2010, and reported at Behrend's website.
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Sometimes one encounters an amplitude spectral density (ASD), which is the square root of the PSD; the ASD of a voltage signal has units of V Hz−1/2. This is useful when the shape of the spectrum is rather constant, since variations in the ASD will then be proportional to variations in the signal's voltage level itself. But it is mathematically preferred to use the PSD, since only in that case is the area under the curve meaningful in terms of actual power over all frequency or over a specified bandwidth. In the general case, the units of PSD will be the ratio of units of variance per unit of frequency; so, for example, a series of displacement values (in meters) over time (in seconds) will have PSD in units of m2/Hz.
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In canonical field theory, the tunneling is described by a wave function which has an amplitude inside the tunnel; but the current is zero there because the relative phase of the amplitude of the conjugate wave function (the time derivative) is orthogonal to it. An electron alt= Another way to look at is: The waves were always on BOTH side of the barrier, but on the right the waves were jiggling in opposite directions. Suppose in the moving illustration on the right, there were another barrier further right and another wave coming FROM the right. The waves in the middle might be stationary if the waves strike the middle at the same time or sometimes jiggling right and sometimes jiggling left depending on which incoming wave gets there most recently.
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From 25 December 2006 to 23 March 2007, photometric observations of Iwamoto were obtained by the international community of photometrists at Badlands Observatory (SD, USA), Ondřejov Observatory (Czech Republic), Modra Observatory (Slovakia), Carbuncle Hill Observatory (RI, USA), Sonoita Research Observatory (AZ, USA), Kharkiv Observatory (Ukraine), McDonald Observatory (TX, USA), Ironwood Observatory (HI, USA), Leura Observatory (Australia), Skalnaté pleso Observatory (Slovakia), Shed of Science Observatory (MN, USA), Pic du Midi Observatory (France). Lightcurve analysis gave a rotation period of 118 hours with a brightness variation of 0.34 magnitude (). In May 2011, astronomers Etienne Morelle, Raoul Behrend obtained another lightcurve with a concurring period of 118 hours and an amplitude of 0.38 magnitude.(). With such a long period, Iwamoto is also a slow rotator, as the vast majority of asteroids have a much shorter rotation period of 2.2 to 20 hours.
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SigSpec (acronym of SIGnificance SPECtrum) is a statistical technique to provide the reliability of periodicities in a measured (noisy and not necessarily equidistant) time series. It relies on the amplitude spectrum obtained by the Discrete Fourier transform (DFT) and assigns a quantity called the spectral significance (frequently abbreviated by “sig”) to each amplitude. This quantity is a logarithmic measure of the probability that the given amplitude level is due to white noise, in the sense of a type I error. It represents the answer to the question, “What would be the chance to obtain an amplitude like the measured one or higher, if the analysed time series were random?” SigSpec may be considered a formal extension to the Lomb-Scargle periodogram, appropriately incorporating a time series to be averaged to zero before applying the DFT, which is done in many practical applications.
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The lower reaches of the Ord River extend from the Parry Creek floodplain northwards to the Cambridge Gulf. The upper reaches of the Ord River are permanently fresh; the lower reaches, when not in flood, become saline due to the tidal cycle which, at the coast, has an amplitude of up to 8 m. Within the site the upstream end of the river channel is around 150 m wide with broad sand and gravel spits, while unstable mud bars and islands characterise the 5 km wide mouth. From the mouth of the Ord River, the site extends northwards around the coast to include the False Mouths of the Ord, consisting of a maze of deltaic channels, intertidal mudflats and low muddy islands, an area which receives only a little fresh water from small and ephemeral creeks.
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Sound generation is carried out through another OS call, OSWORD, which handles a variety of tasks enumerated via a task code placed into the accumulator. All OSWORD calls bear a parameter block used to send and receive multiple data; the address of this block is passed in the X and Y registers, with the low byte in X and the high byte in Y. There are four buffered sound channels three melodic and one noise- based on the sound chip found in the BBC Micro. There is only one waveform for melodic channels; the supported note parameters are pitch, duration, amplitude, envelope selection and various control options. For the amplitude parameter, a zero or negative sets a static amplitude, and a positive value select an amplitude and pitch envelope (a predefined temporal variation) to apply to the note.
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Maelstrom and coastal caves The Moskstraumen is created as a result of a combination of several factors, including tides, strong local winds, position of the Lofoten and the underwater topography; unlike most other major maelstroms, such as Saltstraumen, Gulf of Corryvreckan, Naruto whirlpools, Old Sow whirlpool and Skookumchuck Narrows, it is located in the open sea rather than in a strait or channel. Tides have an amplitude of about and are semi-diurnal at Lofoten, that is they rise twice a day; they are the major contribution to the Moskstraumen. Tides are combined with the northerly Norwegian Sea currents and with storm-induced flow to result in a significant stream, with a reported speed varying between the sources from about and above. Strong topographic enhancement of tidal currents: tales of the Maelstrom (extended version) This flow occurs at the significant depths of about .
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FMX LogoUS Patent and Trademark Office FMX is the name of a commercially unsuccessful noise reduction system developed in the 1980s for FM broadcasting in the United States. FM stereo broadcasting is known to incur up to a 23 dB noise penalty over that of monophonic FM broadcasting; this is due to the combination of the triangular FM noise spectrum and the wider baseband bandwidth occupied by the stereo multiplex signal. Developed at the CBS Technology Center, FMX was intended to improve this characteristic for listeners in the fringe areas where the noise penalty would be worst. This improvement was achieved by adding an amplitude-compressed version of the L−R (left-minus-right, or difference) signal modulated in quadrature with the stereo subcarrier, using a version of the CX noise-reduction system originally developed at CBS for LP records.
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Photo-reflectance is an optical technique for investigating the material and electronic properties of thin films. Photo-reflectance measures the change in reflectivity of a sample in response to the application of an amplitude modulated light beam. In general, a photo-reflectometer consists of an intensity modulated "pump" light beam used to modulate the reflectivity of the sample, a second "probe" light beam used to measure the reflectance of the sample, an optical system for directing the pump and probe beams to the sample, and for directing the reflected probe light onto a photodetector, and a signal processor to record the differential reflectance. The pump light is typically modulated at a known frequency so that a lock-in amplifier may be used to suppress unwanted noise, resulting in the ability to detect reflectance changes at the ppm level.
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Increasing and decreasing trends can continue for periods of a century or more. The Schwabe Cycle is thought to be an amplitude modulation of the 87 year (70–100 year) Gleissberg cycle, named after Wolfgang Gleißberg. The Gleissberg cycle implied that the next solar cycle have a maximum smoothed sunspot number of about 145±30 in 2010 (instead 2010 was just after the cycle's solar minimum) and that the following cycle have a maximum of about 70±30 in 2023. Associated centennial variations in magnetic fields in the Corona and Heliosphere have been detected using Carbon-14 and beryllium-10 cosmogenic isotopes stored in terrestrial reservoirs such as ice sheets and tree rings PDF Copy and by using historic observations of Geomagnetic storm activity, which bridge the time gap between the end of the usable cosmogenic isotope data and the start of modern satellite data.
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They measured a base of 7246 toises near Perpignan, and a somewhat shorter base near Dunkirk; and from the northern portion of the arc, which had an amplitude of 2° 12′ 9″, obtained 56,960 toises for the length of a degree; while from the southern portion, of which the amplitude was 6° 18′ 57″, they obtained 57,097 toises. The immediate inference from this was that, with the degree diminishing with increasing latitude, the earth must be a prolate spheroid. This conclusion was totally opposed to the theoretical investigations of Newton and Huygens, and accordingly the Academy of Sciences of Paris determined to apply a decisive test by the measurement of arcs at a great distance from each other — one in the neighbourhood of the equator, the other in a high latitude. Thus arose the celebrated expeditions of the French academicians to the Equator and to Lapland directed by Pierre Louis Maupertuis.
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Since the 1990s, and up to June 2016, four well-defined rotational lightcurves were obtained for this asteroid from photometric observations, giving a rotation period of approximately 4.95 hours with a high brightness variation between 0.53 and 0.82 in magnitude, indicating that the asteroid has a non-spheroidal shape. In the 1990s, Italian astronomer Stefano Mottola obtained a lightcurve at La Silla during the EUNEASO, a European near-Earth object search and follow-up observation program to determine additional physical parameters (). Further lightcurves were obtained by Polish astronomer Wiesław Z. Wiśniewski at UA's LPL in October 1993, and by Czech astronomer Petr Pravec at Ondřejov Observatory in September 1997 (). In June 2016, the fourth and most recent photometric observation was made by American astronomer Brian Warner at his Palmer Divide Station, Colorado, which gave a period of hours with an amplitude of 0.82 in magnitude ().
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AZ Phoenicis is a Delta Scuti variable that pulsates with a single period of 79.3 minutes, causing its visual brightness to vary with an amplitude of 0.015 magnitudes. Its variability was discovered by Werner Weiss in 1977, from observations with the 50-cm telescope at La Silla Observatory. AZ Phoenicis has also been classified as a possible Ap star, which remains uncertain, even though the star has a large concentration of metals; the overall metallicity of the star has been measured to about 3 times the solar metallicity. This star is classified with a spectral type of A9/F0III, corresponding to a giant of type A or F. With an estimated radius of 2.7 times the solar radius, it is shining with 19 times the solar luminosity at an effective temperature of 7,280 K. The astrometric observations by the Hipparcos spacecraft detected a significant acceleration in the proper motion of AZ Phoenicis, indicating it is an astrometric binary.
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High-precision ephemerides of sun, moon and planets were developed and calculated at the Jet Propulsion Laboratory (JPL) over a long period, and the latest available were adopted for the ephemerides in the Astronomical Almanac starting in 1984. Although not an IAU standard, the ephemeris time argument Teph has been in use at that institution since the 1960s. The time scale represented by Teph has been characterized as a relativistic coordinate time that differs from Terrestrial Time only by small periodic terms with an amplitude not exceeding 2 milliseconds of time: it is linearly related to, but distinct (by an offset and constant rate which is of the order of 0.5 s/a) from the TCB time scale adopted in 1991 as a standard by the IAU. Thus for clocks on or near the geoid, Teph (within 2 milliseconds), but not so closely TCB, can be used as approximations to Terrestrial Time, and via the standard ephemerides Teph is in widespread use.
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It will make it closest approach in around 733,000 years when it comes within . The brighter primary, component A, is an F-type main-sequence star with a stellar classification of F1.5 V. It is a periodic variable star with a frequency of 11.09569 cycles per day (2.16 hours per cycle) and an amplitude of 0.0025 in magnitude. The star has an estimated 1.32 times the mass of the Sun and is radiating nine times the Sun's luminosity from its photosphere at an effective temperature of around 6,863 K. It displays a strong infrared excess at a wavelength of 24 μm and a weaker excess at 70 μm, indicating the presence of a circumstellar disk of dust with a temperature of 188 K, orbiting at 6.7 AU from the host star. The magnitude 9.6 companion, component B, lies at an angular separation of 11.6 arc seconds from the primary as of 2008.
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While total reflection, by definition, involves no continuing flow of power across the interface between the two media, the external medium carries a so-called evanescent wave, which travels along the interface with an amplitude that falls off exponentially with distance from the interface. The "total" reflection is indeed total if the external medium is lossless (perfectly transparent), continuous, and of infinite extent, but can be conspicuously less than total if the evanescent wave is absorbed by a lossy external medium ("attenuated total reflectance"), or diverted by the outer boundary of the external medium or by objects embedded in that medium ("frustrated" TIR). Unlike partial reflection between transparent media, total internal reflection is accompanied by a non-trivial phase shift (not just zero or 180°) for each component of polarization (perpendicular or parallel to the plane of incidence), and the shifts vary with the angle of incidence. The explanation of this effect by Augustin-Jean Fresnel, in 1823, added to the evidence in favor of the wave theory of light.
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A product detector is a type of demodulator used for AM and SSB signals, where the original carrier signal is removed by multiplying the received signal with a signal at the carrier frequency (or near to it). Rather than converting the envelope of the signal into the decoded waveform by rectification as an envelope detector would, the product detector takes the product of the modulated signal and a local oscillator, hence the name. By heterodyning, the received signal is mixed (in some type of nonlinear device) with a signal from the local oscillator, to give sum and difference frequencies to the signals being mixed, just as a first mixer stage in a superhet would produce an intermediate frequency; the beat frequency in this case, the low frequency modulating signal is recovered and the unwanted high frequencies filtered out from the output of the product detector. Because the sidebands of an amplitude-modulated signal contain all the information in the carrier displaced from the center by a function of their frequency, a product detector simply mixes the sidebands down into the audible range so that the original audio may be heard.
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Circulation and transport within the Indonesian Seas vary along with large-scale monsoon flow. During June to August, southeasterlies of the southwest monsoon predominate over Indonesia and drive strong Ekman divergence (southwestward flow in the Southern Hemisphere thus increasing ITF to 15 Sv) whereas from December to February, Northwest Monsoon westerlies serve to directly reduce the ITF. During monsoon transitions, strong westerly winds in the eastern Indian Ocean force equatorial downwelling Kelvin waves (eastward moving, eastward flow) that propagate through the Indonesian passages as coastally trapped Kelvin waves and serve to reduce the ITF flow with a minimum in April of 9 Sv. Another way to think about it is that downwelling on the Indian Ocean side increases sea level and so reduces the normal Pacific-to-Indian pressure head reducing the flow. Global-scale, ocean waves such as equatorial/coastal Kelvin and Rossby waves drive interannual variation of the ITF with an amplitude of roughly +/-3 Sv.Schiller, A., S.E. Wijffels, J. Sprintall, R. Molcard, and P.R. Oke, Pathways of intraseasonal variability in the Indonesian Throughflow region, Dynamics of Atmospheres and Oceans, 50 (2), 174-200, 2010.
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The R, G and B primary color signals are passed through a "matrix" to derive the luminance signal, Y, which is the monochrome equivalent of the three primary colors. With the addition of inputs from the synchronizing generator, which supplies the blanking and composite synch signals, and inputs from the color burst generator, which supplies the 3.579545 MHz color burst and the "burst gate" signals, the colorplexer, using an "encoder", synthesizes a compatible signal which includes luminance (described earlier) and chrominance (an amplitude-modulated suppressed-carrier signal with "I" and "Q" in quadrature, and which represents the differences between the color signals and the monochrome signal), the combination of which produces a monochrome-compatible color information stream. The "burst gate" admits eight cycles of the 3.579545 MHz "color burst" and applies this to the "back porch" of each horizontal synch pulse (the vertical synch is unaffected). These eight cycles are just enough to supply a color TV receiver with a reference with which it can correct its own 3.579545 MHz local oscillator as to frequency and phase, phase being the most significant aspect of the process of recovering the "I" and "Q" signals.
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Mass dampers are frequently implemented with a frictional or hydraulic component that turns mechanical kinetic energy into heat, like an automotive shock absorber. Given a motor with mass m1 attached via motor mounts to the ground, the motor vibrates as it operates and the soft motor mounts act as a parallel spring and damper, k1 and c1. The force on the motor mounts is F0. In order to reduce the maximum force on the motor mounts as the motor operates over a range of speeds, a smaller mass, m2, is connected to m1 by a spring and a damper, k2 and c2. F1 is the effective force on the motor due to its operation. Response of the system excited by one unit of force, with () and without () the 10% tuned mass. The peak response is reduced from 9 units down to 5.5 units. While the maximum response force is reduced, there are some operating frequencies for which the response force is increased. The graph shows the effect of a tuned mass damper on a simple spring–mass–damper system, excited by vibrations with an amplitude of one unit of force applied to the main mass, m1.
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In most cases the signal will actually be B-Format, but in the case of 2-channel UHJ there is insufficient information available to be able to reconstruct a true B-Format signal, only something that behaves in a similar way. The information is then passed to an amplitude matrix that develops the speaker feeds, via a set of shelf filters, which improve the accuracy and performance of the decoder in smaller listening environments (they can be omitted in larger-scale applications). Ambisonics was designed to suit actual living rooms and practical speaker positions: most living rooms are rectangular and as a result the basic system was designed to decode to four loudspeakers in a rectangle, with sides between 1:2 (width twice the length) and 2:1 (length twice the width) in length, thus suiting the majority of living rooms. A layout control is generally provided to allow the decoder to be configured for the loudspeaker positions - an important aspect of Ambisonic replay where it differs from other surround systems: the decoder is specifically configured for the size and layout of the speaker array.
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