I decide to head to Starbucks since it's double-star day.
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The brighter double star Theta1 Orionis C (lower right) is also well seen.
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Double star system Eta Carinae seems perpetually ready to explode, as we've reported before.
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Those halcyon days may be over, but now, we have a double star system to enjoy instead.
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Molnar and his colleagues have identified seven candidate double-star systems in a "penultimate" stage of becoming red novas.
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The latest known red nova was V1309 Scorpii, a double-star system that unexpectedly merged and detonated in 2008.
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What's notable about this particular discovery is that it's the largest planet in a double-star system discovered so far.
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This month, she and her partner of 34 years, Kurt Russell, were honored with a double star on the Hollywood Walk of Fame.
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The astronomers hypothesize that the runaway star was once part of a double-star system that came too close to the black hole.
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The unusually high amount of double star systems demonstrates that Arp 299 includes some of the most prolific star-forming galaxies in the universe.
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The unusually high amount of double star systems demonstrates that Arp 299 includes some of the most prolific star-forming galaxies in the universe.
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"The planets will appear to move past each other forming what looks like a brilliant double star," NASA said in a video touting the event.
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Already, from these first data, GRAVITY made a discovery: one of the components of the cluster (Theta1 Orionis F, lower left) was found to be a double star for the first time.
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Scientists think either binary black holes were formed from a double star system or they are "completely solitary" black holes that end up in a star cluster orbiting one another, LIGO researcher Nergis Mavalvala said.
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Other tweaks include the addition of double-star days (4 stars per $1 spent), and a series of strategic partnerships with technology companies including Spotify and Lyft, which will allow customers to earn stars outside of Starbucks.
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"This means that double-star systems of the type studied here are excellent candidates to host habitable planets, despite the large variations in the amount of starlight hypothetical planets in such a system would receive," said Max Popp, associate research scholar at Princeton University, in a press release.
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Perhaps its most iconic image epitomizes its genius for making the corniest clichés strange and new: a bored kid stuck in a nowhere town looking to the horizon, yearning for better things, no different from Dorothy in dusty Kansas or the teenagers in Modesto, watching the setting of a double star.
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It was included with an 11th-magnitude companion as a double star as H IV 66 in the Herschel Catalogue of Double Stars and Σ II 2 in the Struve Double Star Catalog, and together with a 14th-magnitude star as β 550 in the Burnham Double Star Catalogue.
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Accessed on line August 20, 2008. These discoverer codes can be found in the Washington Double Star Catalog.References and discoverer codes, The Washington Double Star Catalog , United States Naval Observatory. Accessed on line August 20, 2008.
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Double Star is a 1979 board wargame published by Game Designers' Workshop.
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6 Cassiopeiae (6 Cas) is a double star in the constellation Cassiopeia.
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The Washington Double Star Catalog lists four companions within a 2 arcsecond angular radius.
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There are indications that component B may itself be a double star, though this is uncertain.
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HD 219279 is a double star in the equatorial constellation of Aquarius. It has three companions.
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Entry 14396-6050, discoverer code RHD 1AB,The Washington Double Star Catalog , United States Naval Observatory.
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However, the Washington Visual Double Star Catalog gives a magnitude of 11.19 with an angular separation of .
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Modern double star observers have since discarded this designation and prefer the observer abbreviation "DUN", as first adopted in the Washington Double Star Catalog (WDS) as maintained by the US Naval Observatory in Washington, D.C.. Hence, p Eridani is DUN 5, Gamma Crucis / Gacrux is DUN 124, etc.
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NGC 158 is a double star in the Cetus constellation. It was discovered by Wilhelm Tempel in 1882.
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NGC 464 is a double star located in the Andromeda constellation. It was discovered in 1882 by Wilhelm Tempel.
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It also has the Bright Star Catalogue number 1457, the HD number 29139, and the Hipparcos catalogue number 21421, mostly seen in scientific publications. It is a variable star listed in the General Catalogue of Variable Stars, but it is listed using its Bayer designation and does not have a separate variable star designation. Aldebaran and several nearby stars are included in double star catalogues such as the Washington Double Star Catalog as WDS 04359+1631 and the Aitken Double Star Catalogue as ADS 3321\.
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Tau2 Gruis (Tau2 Gruis), is a double star located in the constellation Grus. The somewhat faint double star can be located west of Beta Gruis. As of 2015, the pair had an angular separation of 0.60 arc seconds along a position angle of 176°. The system is 156 light years from Earth.
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Pressey sued Smith in 1887 for royalties. The name "Star" was attributed to the double star arrangement of the spokes.
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HD 37646 is a double star in the northern constellation of Auriga. The pair have an angular separation of 26.005″.
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Hubble image of the Sirius binary system, in which Sirius B can be clearly distinguished (lower left) A binary star is a star system consisting of two stars orbiting around their common barycenter. Systems of two or more stars are called multiple star systems. These systems, especially when more distant, often appear to the unaided eye as a single point of light, and are then revealed as multiple by other means. The term double star is often used synonymously with binary star; however, double star can also mean optical double star.
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HD 130458 is a double star in the southern circumpolar constellation of Apus. The pair have an angular separation of 2.167″.
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HD 180262 is a wide double star in the equatorial constellation of Aquila. The pair have an angular separation of 89.823″.
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NGC 156 is a double star located in the Cetus constellation. It was discovered on 1882 by Ernst Wilhelm Leberecht Tempel.
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Sherburne Wesley Burnham and His Double Star Catalogue, Olin J. Eggen, Astronomical Society of the Pacific Leaflets 6, #295 (November 1953), pp. 354–361, By the time Burnham retired from Yerkes Observatory, he had accumulated material for a revision of his catalogue. This eventually formed part of the 1932 Aitken Double Star Catalogue (ADS), the successor to the BDS.
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The database used to construct this catalog was later transferred from Lick Observatory to the United States Naval Observatory, where it became the basis for the Washington Double Star Catalog.The Washington Double Star Catalog , Brian D. Mason, Gary L. Wycoff, and William I. Hartkopf, astrometry department, United States Naval Observatory; accessed on line July 22, 2008.
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The two stars are very close together (0.2 arcsec away), respectively of magnitude 5.1 and 5.5.The Washington Visual Double Star Catalog (Mason + 2001-2012).Alcyone A third component is located 57 arcsec distant; it is a star of the tenth magnitude, Iota1 Librae B. The third component is also a double star, of equal magnitudes, 1.9 arcseconds apart.
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FK Pohronie B is inactive. Most recently, it had played in the Slovak 7th football level ( VII. liga DOUBLE STAR BET ObFZ ZH).
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In the mathematical field of graph theory, the double-star snark is a snark with 30 vertices and 45 edges. In 1975, Rufus Isaacs introduced two infinite families of snarks—the flower snark and the BDS snark, a family that includes the two Blanuša snarks, the Descartes snark and the Szekeres snark (BDS stands for Blanuša Descartes Szekeres). Isaacs also discovered one 30-vertex snark that does not belongs to the BDS family and that is not a flower snark — the double-star snark. As a snark, the double-star graph is a connected, bridgeless cubic graph with chromatic index equal to 4.
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Only one of these is listed in the Washington Double Star Catalog and Catalog of Components of Double and Multiple Stars as a companion.
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Delta Hydrae, Latinized from δ Hydrae, is a double star in the equatorial constellation of Hydra. It is visible to the naked eye with an apparent visual magnitude of 4.146. Based upon an annual parallax shift of 20.34 mas, it is located about 160 light years from the Sun. This is a double star with an angular separation of along a position angle of , as of 2003.
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It is separated from ι Boo by 1,100 AU. The Washington Double Star Catalog lists a third component, a 14th magnitude star at 90 arc seconds.
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68 Aquilae (abbreviated 68 Aql) is a double star in the equatorial constellation of Aquila. 68 Aquilae is its Flamsteed designation. Its apparent magnitude is 6.12.
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Component B shares a common linear motion through space with the primary, and thus may form a third member of the system. This star has 0.84 times the mass of the Sun and a projected separation of from the primary. The Washington Double Star Catalogue has it classified as a double star, with a magnitude 11.30 companion at an angular separation of along a position angle of 292°, as of 2002.
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The comet became visible to the naked eye from dark-sky sites around February 7. It figured near the double star Zubenelgenubi on February 6, near Spica on February 15 and 16, near Gamma Virginis on February 19 and near the star cluster M44 on March 5 and 6. It also figured near the planetary nebula NGC 2392 on March 14, and near the double star Wasat around March 17.
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The star is radiating 913 times the luminosity of the Sun from its photosphere at an effective temperature of 13,175 K; this searing heat gives it the blue- white glow of a B-type star. 21 Aquilae is catalogued as an optical double star, having a 12th magnitude companion away as of 2010. It was first identified as a double star by John Herschel. The companion is a distant background object.
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The Cluster Science Archive is the ESA long term archive of the Cluster and Double Star science missions. Since 1 November 2014, it is the sole public access point to the Cluster mission scientific data and supporting datasets. The Double Star data are publicly available via this archive. The Cluster Science Archive is located alongside all the other ESA science archives at the European Space Astronomy Center, located near Madrid, Spain.
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Amateur telescopes can discern them but require magnification of about 100 times. They are situated 50′ east of the well-known double star system Gamma Leonis (i.e. Algieba).
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Admiral William Henry Smyth was the first to see the 10.8-magnitude red giant, citing the double star on Cassiopeia's knee, about a degree to nf of Delta.
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HD 151566 is double star in the southern constellation of Ara. As of 1991, the pair had an angular separation of 3.10″ along a position angle of 42°.
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HD 141846 is a double star in the southern constellation of Apus. As of 1996, the pair have an angular separation of 0.7″ along a position angle of 332°.
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HD 215114 is a double star in the equatorial constellation of Aquarius. As of 2012, the pair have an angular separation of 2.29″ along a position angle of 306.4°.
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HD 191984 is a double star in the equatorial constellation of Aquila. As of 2011, the components have an angular separation of 2.52″ along a position angle of 205.7°.
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HD 130603 is a double star in the northern constellation of Boötes. As of 2010.476, the components have an angular separation of 2.06″ along a position angle of 54.7°.
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HD 153221 is a double star in the southern constellation of Ara. As of 2012, the pair have an angular separation of 1.10″ along a position angle of 172°.
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HD 165493 is double star in the southern constellation of Ara. As of 2011, the two components have an angular separation of 4″ along a position angle of 257°.
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3 Geminorum is also a close double star. The brighter component is the variable blue supergiant. The companion is 2.5 magnitudes fainter. The separation is about 0.6 arc- seconds.
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Albireo A and B Beta Cygni is about away from the Sun. When viewed with the naked eye, Albireo appears to be a single star. However, in a telescope it resolves into a double star consisting of β Cygni A (amber, apparent magnitude 3.1), and β Cygni B (blue-green, apparent magnitude 5.1). Separated by 35 seconds of arc,Entry, The Washington Double Star Catalog, identifier 19307+2758, discoverer identifier STFA 43.
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The poles can be varied at a ratio of 1:2 and thus the speed can be varied at 2:1. Normally, the electrical configuration of windings is varied from a delta connection (Δ) to a double star connection (YY) configuration in order to change the speed of the motor for constant torque applications, such as the hoists in cranes. Star connections (Y) varied to double star connections (YY) are used for quadratic torque applications, such as pumps.
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Gamma Leporis is a double star divisible in binoculars. The primary is a yellow star of magnitude 3.6, 29 light-years from Earth. The secondary is an orange star of magnitude 6.2.
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HD 156331 is double star in the southern constellation of Ara. As of 2014, the pair have an angular separation of less than an arc second along a position angle of 49°.
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HD 150576 is a double star in the southern constellation of Ara. It has a twelfth magnitude companion at an angular separation of 28.3″ along a position angle of 39° (as of 2000).
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4 Aurigae is a double star at a distance of 159 light-years. The primary is of magnitude 5.0 and the secondary is of magnitude 8.1. 14 Aurigae is a white optical binary star.
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Entry 17318-4953, The Washington Double Star Catalog , United States Naval Observatory. Accessed on line November 26, 2008. The two stars appear close to each other by coincidence and are not physically close in space.
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The Neelanjali Ruby, at 1,370 carats (274 g), is the world's largest double- star ruby. A ruby is known as a star ruby if it contains an asterism (distinctive star-shaped light refraction) in the gem. The Neelanjali Ruby is the world's largest star ruby with a 12-point asterism, which is commonly denoted as a double-star ruby. The Neelanjali ruby, along with the Rajarathna ruby, was used as a Shiva lingam and was worshipped for centuries in the home of the family which owned it.
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Winnecke 4 (also known as Messier 40 or WNC 4) is an optical double star consisting of two unrelated stars in the constellation Ursa Major. WNC 4 was discovered by Charles Messier in 1764 while he was searching for a nebula that had been reported in the area by Johannes Hevelius. Not seeing any nebulae, Messier catalogued this double star instead. It was subsequently rediscovered by Friedrich August Theodor Winnecke in 1863, and included in the Winnecke Catalogue of Double Stars as number 4.
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It has a mass of 46 . The primary may itself be a double star, suggested by the improbably large mass found from the binary orbit when compared to the other stellar parameters. The Washington Double Star Catalog lists 11 companions within one arc minute of HD 15558 A, all fainter than 10th magnitude. In addition, it lists component E just over one arc minute away; it is another hot massive star, the 9th magnitude BD+60°501 with a spectral type of O7 V(n)((f))z.
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Gamma Equulei, Latinized from γ Equulei, is a double star in the northern constellation of Equuleus. It is located at a distance of around from Earth and has a slightly variable apparent visual magnitude around 4.7.
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He performed experiments to study how such craters might have formed. Hooke also was an early observer of the rings of Saturn, and discovered one of the first observed double-star systems, Gamma Arietis, in 1664.
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HD 132029 is a star in the northern constellation of Boötes. It forms a double star with a magnitude 10.2 companion at an angular separation of 4.6″ along a position angle of 110° (as of 2010).
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See The Binary Stars, Robert Grant Aitken, New York: Dover, 1964, pp. 24–25, 38, and p. 61, The present status of double star astronomy, K. Aa. Strand, Astronomical Journal 59 (March 1954), pp. 61–66, .
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Sparrow's resolution limit was derived in 1916 from photographic experiments with simulated spectroscopic lines and is most commonly applied in spectroscopy, microscopy and photography. The Dawes resolution limit is more often used in visual double star astronomy.
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Mintaka (δ Orionis) is 1,200 light-years away and shines with magnitude 2.21. Mintaka is 90,000 times more luminous than the Sun. Mintaka is a double star. The two stars orbit around each other every 5.73 days.
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GSC 02620-00648 is a double star in the constellation Hercules. The brighter of the pair is a magnitude 12 star located approximately 1400 light-years away. This star is about 1.18 times as massive as the Sun.
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HD 33203 is double star in the northern constellation of Auriga. It includes a bright giant star with a stellar classification of B2II. The two components have an angular separation of 1.617″ along a position angle of 222.1°.
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He was one of the founders of the British Astronomical Association, and served as its Double Star Section Director from 1892 to 1915, its Saturn Section Director from 1899 to 1911, and its president from 1900 to 1902.
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The stars 30 and 31 Cygni form a contrasting double star similar to the brighter Albireo. The two are visible in binoculars. The primary, 31 Cygni, is an orange-hued star of magnitude 3.8, 1400 light-years from Earth.
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HD 24480 is a double star in the northern constellation of Camelopardalis. The brighter component is a giant star with a stellar classification of K4III and an apparent magnitude of 5.20. The pair have an angular separation of 1.71″.
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The pair complete an orbit around the primary star every 24,762 years. Catalogues of stellar multiplicity, like the Washington Double Star Catalog, usually list another component; this star, however, is located much more far away than the other two.
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HD 152082 is an A-type shell star in the southern constellation of Ara. This is a double star with a thirteenth magnitude companion at an angular separation of 6.8″ along a position angle of 329° (as of 2000).
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The Washington Visual Double Star Catalog lists five visual companions within 100″; the closest and brightest such companion is the magnitude 8.6 θ Geminorum E at an angular separation of 2.4″ along a position angle of 295°, as of 2010.
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45 Andromedae, abbreviated 45 And, is a double star in the northern constellation Andromeda. 45 Andromedae is the Flamsteed designation. Its combined apparent visual magnitude is 5.80. Based upon an annual parallax shift of , it is located 341 light years away.
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HD 35619 is a double star in the northern constellation of Auriga. It has an apparent magnitude of 8.572, which is too faint to be viewed with the naked eye. The companion is 12th magnitude and 2 arc-seconds away.
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HR 2096, also known as HD 40325 is a double star in the constellation Auriga. It is composed of two ageing orange giants of spectral types K0III and K2III. It is not a member of any known moving group of stars.
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The Washington Double Star Catalog lists a 16th magnitude companion as component C and a 10th magnitude companion as component D. Component D is HD 236848 and it shares the same space motion and distance as the inner three stars.
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The Chinese ox star (or constellation) corresponds more-or-less with the constellation Capricornus. The Ox mansion (牛宿, pinyin: Niú Xiù) is one of the Twenty-eight mansions of the Chinese constellations. It is one of the northern mansions of the Black Tortoise. The determinative star is beta Capricorni (β Capricorni), known as 牛宿一 (Niú Su yī, literally, the First Star of Ox); or, rather, β Capricorni appears to be a star, to the naked eye, but actually resolves into double star systems, according to modern astronomy, and even with just slight magnification appears to be a double star.
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Xi Phoenicis is known as a double star since 1834, the date of the first registered observation in the Washington Double Star Catalogue. The relative position of the two components has remained constant to this day, confirming they have a common proper motion and form a physical binary system. The secondary star has a visual apparent magnitude of 9.95 and in 2007 was located at an angular separation of 13.06 arcseconds and position angle of 252.5°, in relation to the primary. Considering the distance to the system, this corresponds to a projected separation of 875 AU between the stars.
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It forms part of a double star along with a fainter optical companion designated Gamma¹ Sagittarii located about 50 arcminutes north of this star. The latter is a magnitude 4.7 Cepheid variable star that also has the variable star designation W Sagittarii.
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HD 82205 is a double star in the southern constellation of Antlia. However, the primary is most likely a solitary star as the other component is deemed a line of sight companion. This is a giant star with a stellar classification of K3III.
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The catalogue later became the Washington Double Star Catalog. Van den Bos developed his own method of measuring the orbits of double stars and used it to measure the orbits of more than 100 binary stars. His method became the accepted standard procedure.
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Eta Andromedae has a visual companion star of apparent visual magnitude 11.5, BD+22°153B, visible 129.2 arcseconds away.Entry 00572+2325, discoverer code FOX 116, components AB, The Washington Double Star Catalog , United States Naval Observatory. Accessed on line August 23, 2008.
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From 1918 to 1928, he was chair of the double star committee for the International Astronomical Union. Aitken was partly deaf and used a hearing aid. He married Jessie Thomas around 1888, and had three sons and one daughter. Jessie died in 1943.
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Double Star is a science fiction novel by American writer Robert A. Heinlein, first serialized in Astounding Science Fiction (February, March, and April 1956) and published in hardcover the same year. It received the 1956 Hugo Award for Best Novel (his first).
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The Washington Double Star Catalog lists two 14th magnitude companions about away. In addition, an unseen close companion is suspected due to some faint emission lines in the spectrum that are best explained by a Be star invisible against the brighter primary.
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In the List, the components are clearly identified by their identifiers in the Washington Double Star Catalog. Where a component letter is not explicitly listed, the WGSN says that the name should be understood to be attributed to the visually brightest component.
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M103 is far poorer than M52, with only about 25 stars included. It is also more distant, at 8200 light- years from Earth. Its most prominent member is actually a closer, superimposed double star; it consists of a 7th-magnitude primary and 10th-magnitude secondary.
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Besides being a critic of poetry and culture in general, Komrij wrote several semi-autobiographical works, including Verwoest Arcadië ('Arcadia Demolished', 1980) and Demonen ('Demons', 2003). He also authored several novels, Over de bergen ('Over the Mountains'), Dubbelster ('Double Star') and De klopgeest ('Poltergeist').
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HD 131040 is a double star in the northern constellation of Boötes. The brighter component is a subgiant star that varies slightly in luminosity by 0.04 in magnitude. The magnitude 9.64 companion lies at an angular separation of 15.2″ along a position angle of 93°.
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Gamma Draconis has six companions listed in double star catalogues. All were discovered by the American astronomer Sherburne Wesley Burnham. The closest may be physically associated and would be separated by about . The luminosity of this object suggests it is a red dwarf star.
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HD 153791 is a double star in the southern constellation of Ara. The primary is a sixth magnitude A-type main sequence star. It has a magnitude 12.3 companion at an angular separation of 6.0″ along a position angle of 249°, as of 1999.
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Gamma Tauri (γ Tauri, abbreviated Gamma Tau, γ Tau) is either a solitary, binary or double star (the Washington Double Star Catalog notes it as a "Dubious Double" or "Bogus Binary") that marks the tip of the "V" in the constellation of Taurus. It is a member of, and located within about 2.5 parsecs of the center of, the Hyades star cluster, the nearest open cluster to the Sun. Based upon parallax measurements, Gamma Tauri is approximately 154 light-years from the Sun. Considered as a pair of stars, the two components are designated Gamma Tauri A (officially named Prima Hyadum , the traditional name for the system) and B.
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HD 16028 is a star in the constellation Andromeda. Its apparent magnitude is 5.71. Located approximately distant, it is an orange giant of spectral type K3III, a star that has used up its core hydrogen and has expanded. Double star catalogues list two stars as optical companions.
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Gamma Boötis forms the primary or 'A' component of a double star system designated WDS J14321+3818 ('B' is the star UCAC2 45176266). Gamma Boötis' two components are themselves designated WDS J14321+3818Aa (officially named Seginus , the traditional name of the Gamma Bootis system) and Ab.
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It is often considered by stargazers to be a beautiful double star with a striking contrast of color. It was later discovered that γ2 Andromedae is itself a triple star system. What appears as a single star to the naked eye is thus a quadruple star system.
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The visual binary nature of HD 205877 was discovered by the Hipparcos spacecraft and given the double star discoverer designation HDS 3084. The preliminary orbital elements of the system were determined with speckle interferometric measurements made at the 4.1 m Southern Astrophysical Research Telescope in Chile.
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Gamma1 Fornacis (γ1 For) is a star in the constellation Fornax. Its apparent magnitude is 6.15. It is a yellow giant that has swollen and brightened to around 80 times as luminous as the Sun. γ1 Fornacis has three companions listed in the Washington Double Star Catalog.
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The traditional name "Deneb Kaitos" means "the whale's tail". γ Ceti, Kaffaljidhma ("head of the whale") is a very close double star. The primary is a yellow- hued star of magnitude 3.5, 82 light-years from Earth, and the secondary is a blue-hued star of magnitude 6.6.
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The other bright star in Chamaeleon is Delta Chamaeleontis, a wide double star. The brighter star is Delta2 Chamaeleontis, a blue-hued star of magnitude 4.4. Delta1 Chamaeleontis, the dimmer component, is an orange-hued giant star of magnitude 5.5. They both lie about 350 light years away.
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Unique Details Of Double Star In Orion Nebula And Star T Leporis Captured By 'Virtual' Telescope. ScienceDaily. Retrieved February 19, 2009, RX Leporis is a semi-regular red giant that has a period of 2 months. It has a minimum magnitude of 7.4 and a maximum magnitude of 5.0.
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HD 208177 is a double star system in the equatorial constellation of Aquarius. They are faintly visible to the naked eye with an apparent magnitude of 6.20. The pair have an angular separation of 19.113″. The primary component is an evolved subgiant star with a stellar classification of F5IV.
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HD 187734 is double star in the equatorial constellation of Aquila. The primary is a magnitude 6.6 giant star, while the companion is a magnitude 9.4 A-type main sequence star. As of 2014, the pair had an angular separation of 5″ along a position angle of 99°.
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Epsilon Draconis is resolvable as a double star in telescopes of 10 centimeters aperture or larger. The companion has an apparent brightness of 7.3 at an angular distance of 3.2 arcseconds. It is a giant of spectral class F5, orbiting the yellow giant at about 130 astronomical units.
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The cover illustration for a 1970s UK edition of Double Star (artist: Anthony Roberts) was the subject of an unlikely controversy when it was used as the basis of an entry for the 2000 Turner Prize for modern art. The artist in question, Glenn Brown, was accused of plagiarism.
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All 3371 publications related to the Cluster and the Double Star missions (count as of 31 August 2020) can be found on the publication section of the ESA Cluster mission website. Among these publications, 2886 are refereed publications, 342 proceedings, 113 PhDs and 30 other types of theses.
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NGC 1995 (also known as PGC 3325910) is a double star located in the Pictor constellation. It was discovered by John Herschel on December 28, 1834. Its size is 0.78 arc minutes. In some sources, such as VizieR, NGC 1995 is misidentified as nearby Lenticular galaxy NGC 1998.
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The Big Dipper's bowl and part of the handle photographed from the International Space Station. Mizar and Alcor are at the upper right. The multiple star system of Mizar (the double star on the right) and Alcor (left). The unrelated, fainter star Sidus Ludovicianum can be seen lower down.
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Kappa Tauri (κ Tau, κ Tauri) is a double star in the constellation Taurus, the two components κ1 Tauri and κ2 Tauri both members of the Hyades open cluster. The pair are approximately 150 light years from Earth and are separated from each other by about six light years.
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HD 222399 is a double star in the northern constellation of Andromeda. The magnitude 6.57 primary is an F-type subgiant star with a stellar classification of F2IV. It has a magnitude 10.57 companion at an angular separation of 14.7″ along a position angle of 162° (as of 2002).
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HD 156768 is a double star in the southern constellation of Ara. The brighter component is a sixth magnitude bright giant or supergiant star with a stellar classification of G8Ib/II. The magnitude 9.6 companion lies at an angular separation of 1.81″ along a position angle of 184°.
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Gamma1 Caeli, Latinized from γ1 Caeli, is a double star in the constellation Caelum. It is approximately 185 light years from Earth. The brighter component is an orange K-type giant with an apparent magnitude of +4.55. The companion is an eighth magnitude star located 3.1 arcseconds away.
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The three stars of θ2 Orionis within the Orion Nebula θ2 Orionis consists of three stars in a line, each about an arc-minute from the next. In addition to the well-known three stars, the Washington Double Star Catalog confusingly lists a component D which is actually θ1 Orionis C. There is one other star brighter than 10th magnitude in the region. V1073 Orionis is a B9.5 Orion variable that forms an equilateral triangle with θ2 Ori B and C. Bizarrely, θ2 Orionis C has a second entry in the Washington Double Star Catalog under the name S490. The companion is 10th magnitude and actually lies between θ2 Ori B and V1073 Ori.
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Since this time, many more double stars have been catalogued and measured. The Washington Double Star Catalog, a database of visual double stars compiled by the United States Naval Observatory, contains over 100,000 pairs of double stars,"Introduction and Growth of the WDS", The Washington Double Star Catalog , Brian D. Mason, Gary L. Wycoff, and William I. Hartkopf, Astrometry Department, United States Naval Observatory, accessed on line August 20, 2008. including optical doubles as well as binary stars. Orbits are known for only a few thousand of these double stars,Sixth Catalog of Orbits of Visual Binary Stars , William I. Hartkopf and Brian D. Mason, United States Naval Observatory, accessed on line August 20, 2008.
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KOI-256 is a double star located in the constellation Cygnus approximately from Earth. While observations by the Kepler spacecraft suggested the system contained a gas giant exoplanet orbiting a red dwarf, later studies determined that KOI-256 was a binary system composed of the red dwarf orbiting a white dwarf.
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NGC 18 is a double star system (both G4) system located in the constellation of Pegasus. It was first recorded by Herman Schultz on 15 October 1866. It was looked for but not found by Édouard Stephan on 2 October 1882. It was independently observed by Guillaume Bigourdan in November 1886.
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NGC 510 was discovered by Swedish astronomer Herman Schultz on November 11, 1867. The object was initially considered a "misty" object (a galaxy) based on the observations with research instruments of that time, and was included on the NGC list. Later it became clear that it was a double star.
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Delta Sagittarii (δ Sagittarii, abbreviated Delta Sgr, δ Sgr), formally named Kaus Media , is a double star in the southern zodiac constellation of Sagittarius. The apparent visual magnitude of this star is +2.70, making it easily visible to the naked eye. Parallax measurements place the distance at roughly from the Sun.
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NGC 7243 (also known as Caldwell 16) is an open cluster and Caldwell object in the constellation Lacerta. It shines at magnitude +6.4. Its celestial coordinates are RA , dec . It is located near the naked-eye stars Alpha Lacertae, 4 Lacertae, an A-class double star, and planetary nebula IC 5217.
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HD 128093 is a double star in the constellation Boötes. The brighter component is an F-type main sequence star with a stellar classification of F5V and an apparent magnitude of 6.33. It has a magnitude 11.33 companion at an angular separation of 28.1 along a position angle of 318°.
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HD 95808 is a double star in the constellation of Crater. Its apparent magnitude is 5.50, but interstellar dust makes it appear 0.11 magnitudes dimmer than it should be. It is located some 340 light-years (104 parsecs) away, based on parallax. HD 95808 is a G-type giant star.
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The Zeiss can show the daily motions of the sky, the sun, the moon, and the positions of the stars on almost any given day, as well as various astronomical grids and scales. Auxiliary equipment allows projection of rainbows, clouds, solar and lunar eclipses, rotating galaxies, double star systems, and varied constellations.
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1 Arietis is a double star in the northern constellation of Aries. 1 Arietis is the Flamsteed designation. The pair have a combined visual magnitude of 5.86, making it faintly visible to the naked eye. Based upon an annual parallax shift of 5.57 mas, the distance to the two stars is approximately .
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Kappa Boötis (κ Boo, κ Boötis) is a double star in the constellation Boötes. It has the traditional name Asellus Tertius (Latin for "third donkey colt")Star Name - R.H.Allen p.105 and the Flamsteed designation 17 Boötis. The components are separated by an angular distance of 13.5 arcsec, viewable in a small telescope.
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57 Aquilae (abbreviated 57 Aql) is a double star in the constellation of Aquila. 57 Aquilae is its Flamsteed designation. The primary star has an apparent visual magnitude of 5.70, while the secondary is magnitude 6.48. The pair have an angular separation of 35.624 arcseconds and probably form a wide binary star system.
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The catalog was a successor to the Burnham Double Star Catalogue and was based on observations compiled by Sherburne Wesley Burnham from 1906 to 1912, and by Eric Doolittle from 1912 to 1919. Aitken began work on the catalog shortly after Doolittle's death in 1920. The catalog contains observations made up to 1927.
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Despite this, he still makes dolls, for it is his way of proving to himself that he can make people happy. And the dolls he made serve as 'evidences of his existence'. He is also the creator of Mr. Bear. He belongs to the Technical Class, and is currently a Double Star.
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HD 127304 is a double star in the northern constellation of Boötes. The brighter component is a sixth magnitude A-type main sequence star with a stellar classification of A0Vs It has a faint magnitude 10.62 companion at an angular separation of 25.6″ along a position angle of 256° (as of 2013).
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The angle between the two components is 1°. Mesarthim was discovered to be a double star by Robert Hooke in 1664, one of the earliest such telescopic discoveries. The primary, γ1 Arietis, is an Alpha² Canum Venaticorum variable star that has a range of 0.02 magnitudes and a period of 2.607 days.
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It is a yellow giant of magnitude 2.8, 148 light- years from Earth; kornephoros means club-bearer. Delta Herculis A is a double star divisible in small amateur telescopes. The primary is a blue-white star of magnitude 3.1, and is 78 light-years from Earth. The optical companion is of magnitude 8.2.
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Paul Achille‐Ariel Baize (11 March 1901 – 6 October 1995) was a French pediatrician and amateur astronomer specialising in double star observations. He started with his observations of double stars in 1925. Between 1933 and 1971 he was allowed to observe from the Paris Observatory. He made 20,044 measures over 47 years.
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It is visible only with binoculars or better equipment. Components A and B share common proper motion, which confirms them as a physical pair. The projected separation between the stars is 515 AU, but the true separation may be much higher. There is yet another, magnitude 14.4 component listed in the Washington Double Star Catalog.
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HD 88836 is a double star in the southern constellation of Antlia. With an apparent magnitude of 6.35, it is faintly visible to the naked eye from dark skies. The brighter component is a giant star with a stellar classification of G8III. It is radiating energy at a luminosity 58 times that of the Sun.
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HD 220766 is a double star in the equatorial constellation of Aquarius. The primary is a K-type giant star with a stellar classification of K0III and an apparent magnitude of 6.44. It has a faint, magnitude 12 companion, located at an angular separation of 5.0″ along a position angle of 132° (as of 1933).
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107 Aquarii (abbreviated 107 Aqr) is a double star in the equatorial constellation of Aquarius. 107 Aquarii is the Flamsteed designation, although it also bears the Bayer designation i2 Aquarii. The pair have an angular separation of 6.787 arcseconds. They have a combined apparent visual magnitude of +5.305, with individual magnitudes of 5.72 and 6.72.
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33–34, The Binary Stars, Robert Grant Aitken, New York: Dover Publications, Inc., 1964. The second part contains measures, notes, and references to publications for each pair. Its publication was a stimulus to double star observation. The BDS was compiled by Sherburne Wesley Burnham, who worked on it sporadically for 36 years, starting in 1870.
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Kappa Leonis, Latinized from κ Leonis, is a double star in the constellation Leo. It was called Al-minħar al-asad, meaning the Lion's nose. The name is corrupted as Al Minliar al Asad in the Yale Bright Star Catalogue. This star is visible to the naked eye with an apparent visual magnitude of 4.46.
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In the Washington Double Star Catalog HR 8768 has a faint optical companion star with an apparent magnitude of 9.88, from HR 8768. The separation has decreased from when it was discovered as a double in 1828. The two stars share the same Hipparcos identifier HIP 113802, and have very similar parallaxes and proper motions.
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HD 156091 is a double star in the southern constellation of Ara. The primary is a sixth magnitude giant star with stronger than normal lines of carbon, nitrogen, and barium in its spectrum. The companion is a 13th magnitude star at an angular separation of 27.4″ along a position angle of 275°, as of 2000.
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The secondary appears to be of magnitude 6.5, but is actually a close double star itself with a primary of magnitude 7.0 and a secondary of magnitude 7.6. The secondary and tertiary stars have an orbital period of 260 years. The primary has an absolute magnitude of 2.6 and is of spectral class F0.
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The primary and secondary stars are separated by 38.5 arcseconds, at an angle of 33 degrees. The primary and tertiary stars are separated by 86.7 arcseconds at an angle of 194 degrees. Both the primary and tertiary appear white in a telescope, but the secondary appears yellow-hued. Kappa Boötis is another wide double star.
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41 Lyncis is listed in the Washington Double Star Catalog as having two visual companions, the 8th magnitude F-type subgiant HD 81704 away, and an 11th magnitude star away. Both are background objects, more distant than 41 Lyncis itself, but the two share a common proper motion and are at the same distance as each other.
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22 Tauri is a component of the Asterope double star in the Pleiades open cluster. 22 Tauri is the stars' Flamsteed designation. It is situated near the ecliptic and thus is subject to lunar occultation. The star has an apparent visual magnitude of 6.43, which is near the lower threshold of visibility to the naked eye.
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The primary and secondary are both blue-white hued stars of magnitude 2.9; their period is 84 years. Centaurus also has many dimmer double stars and binary stars. 3 Centauri is a double star with a blue-white hued primary of magnitude 4.5 and a secondary of magnitude 6.0. The primary is 344 light-years away.
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Science fiction writer Robert A. Heinlein described therapeutic waterbeds in his novels Beyond This Horizon (1942), Double Star (1956), and Stranger in a Strange Land (1961). In 1980 Heinlein recalled in Expanded Universe: Heinlein made no attempt to build his invention, but its first builder, Charles Hall, was denied a patent claim based on Heinlein's "prior works".
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Delta Boötis (δ Boo, δ Boötis) is a double star in the northern constellation Boötes. Based upon parallax measurements, it is located at a distance of approximately from the Earth. This star is sometimes called Princeps , meaning prince or prime in Latin. The origin of this name is unclear, although it usually appears in an astrological context.
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39 Andromedae, abbreviated 39 And, is a double star in the northern constellation Andromeda. 39 Andromedae is the Flamsteed designation. Its apparent visual magnitude is 5.95, which indicates it is near the lower limit on visibility to the naked eye. The distance to this star, as estimated from its annual parallax shift of , is 341 light years.
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D Centauri (D Cen) is a double star in the constellation Centaurus. The system has a combined apparent magnitude of +5.31 and is approximately 570 light years from Earth. The system is classified as an orange K-type giant. The brighter component has an apparent magnitude of +5.31, while the apparent magnitude of the optical companion is +6.8.
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Parallax measurements show this star to be about 47 light years from the Solar System. The photosphere shows an effective temperature of 5,625 °K and a metallicity (Fe/H) equal to . The Washington Visual Double Star Catalog for 1996 showed two visual companions of this star. The first is a visual magnitude 9.7 star located 289.1 arc seconds away.
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Epsilon2 Arae (ε2 Arae, ε2 Ara) is the Bayer designation for a double star in the southern constellation of Ara. It is approximately distant from Earth. With an apparent visual magnitude of 5.3, it is faintly visible to the naked eye. The brighter star is a magnitude 5.44 F-type main sequence star with a stellar classification of .
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V533 Carinae is the brightest star in the region. The other bright stars in NGC 3572 are hot young stars such as HD 97166 and all the clusters in the region are only a few million years old. V533 Carinae is classified as a double star with the companion being a magnitude 11.5 star 21.7 arc-seconds away.
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By Kőnig's line coloring theorem every bicubic graph has a Tait coloring. The bridgeless cubic graphs that do not have a Tait coloring are known as snarks. They include the Petersen graph, Tietze's graph, the Blanuša snarks, the flower snark, the double-star snark, the Szekeres snark and the Watkins snark. There is an infinite number of distinct snarks..
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"Introduction and Growth of the WDS", The Washington Double Star Catalog , Brian D. Mason, Gary L. Wycoff, and William I. Hartkopf, Astrometry Department, United States Naval Observatory, accessed on line August 20, 2008.Sixth Catalog of Orbits of Visual Binary Stars , William I. Hartkopf and Brian D. Mason, United States Naval Observatory, accessed on line August 20, 2008.
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UZ Pyxidis (HD 75021) is a semiregular variable star in the constellation Pyxis. It is located about 6,000 light-years (2,000 parsecs) away from the Earth. UZ Pyxidis lies directly between α and γ Pyxidis. It has a common proper motion companion, HD 75022, less than 2' away but the two are not listed in double star catalogues.
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However, its most prominent member, the double star Phi Cassiopeiae, is far closer – between 1000 and 4000 light-years away. NGC 457 is fairly rich; it is a Shapley class e and Trumpler class I 3 r cluster. It is concentrated towards its center and detached from the star field. It contains more than 100 stars, which vary widely in brightness.
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1 Camelopardalis (1 Cam) is a double star system in the constellation Camelopardalis. Its combined apparent magnitude is 5.56 and it is approximately away. The 1 Camelopardalis system is part of the Camelopardalis OB1 stellar association, which is 820 pc away. 1 Camelopardalis A is a hot massive star which has evolved away from the main sequence to become a giant.
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Gamma Circini, Latinized from γ Circini, is a star system in the constellation Circinus. It was noted as a double star by Herschel in 1835, who estimated the separation as 1 arc second. It is visible to the naked eye with an apparent visual magnitude of 4.51. Based upon an annual parallax shift of 7.27 mas, it is about 450 light years away.
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HR 4180 is a double star with components HD 92449 and HD 92463 in the southern constellation of Vela. They are probably members of a binary star system. HR 4180 can be viewed with the naked eye, having an apparent visual magnitude of 4.29. Based upon an annual parallax shift of , it is located 640 light years from the Sun.
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66 Arietis (abbreviated 66 Ari) is a double star in the northern constellation of Aries. 66 Arietis is the Flamsteed designation. It has an apparent visual magnitude of 6.03, putting it near the limit for naked eye visibility. The magnitude 10.4 companion is located at an angular separation of 0.810 arcseconds from the primary along a position angle of 65°.
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Omega Aurigae, Latinized from ω Aurigae, is the Bayer designation for a double star in the northern constellation of Auriga. Its apparent magnitude is 4.95, which is bright enough to be seen with the naked eye. The distance to this system, as determined using parallax measurements, is approximately . The system is a member of the Columba group of co-moving stars.
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HD 34557 is a double star in the northern constellation of Auriga. The fainter star has an angular separation of 0.380″ from the primary component. They have a combined apparent magnitude of 5.52, making HD 34557 faintly visible to the naked eye from dark skies. Based upon parallax measurements made with the Hipparcos satellite, this system is roughly 280 light years away.
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Sigma Aquarii (σ Aqr, σ Aquarii) is the Bayer designation for a double star in the equatorial constellation of Aquarius. It is visible to the naked eye with an apparent visual magnitude of 4.81. Based upon parallax measurements, the distance to this star is roughly . Sigma Aquarii has a stellar classification of A0 IVs, indicating that it is a subgiant star.
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The primary, designated component A, has a stellar classification of B9III, matching a blue giant. The magnitude 8.34 secondary, component B, is an A-type main-sequence star of class A7V. A third star of 10th magnitude, BD+77 763, is listed as component C in the Washington Double Star Catalog although it is a background object unrelated to the other two.
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The primary itself is a wide double star with a separation of 25.2 arcseconds; the tertiary has a magnitude of 10.8. The primary and secondary are separated by 3.2 arcseconds. Most of the other stars in Aries visible to the naked eye have magnitudes between 3 and 5. δ Ari, called Boteïn, is a star of magnitude 4.35, 170 light-years away.
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The distribution of the objects of the catalog over the firmament is fairly even. The Washington Double Star Catalog, or WDS, is a catalog of double stars, maintained at the United States Naval Observatory. The catalog contains positions, magnitudes, proper motions and spectral types and has entries for (as of June 2017) 141,743 pairs of double stars. The catalog also includes multiple stars.
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The primary is a silvery giant of magnitude 4.9, and the secondary is an old, reddish giant star of magnitude 5.2. The star HD164669 near the primary may be an optical double. 100 Herculis is a double star easily divisible in small amateur telescopes. Both components are magnitude 5.8 blue-white stars; they are 165 and 230 light-years from Earth.
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The center of mass of the Jupiter–Sun system lies outside the surface of the Sun, though arguing that Jupiter and the Sun are a double star is not analogous to arguing Pluto-Charon is a double dwarf planet. Jupiter is too light to be a fusor; were it thirteen times heavier, it would achieve deuterium fusion and become a brown dwarf.
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Stranger in a Strange Land contains an early description of the waterbed, an invention that made its real-world debut in 1968. Charles Hall, who brought a waterbed design to the United States Patent Office, was refused a patent on the grounds that Heinlein's descriptions in Stranger in a Strange Land and another novel, Double Star (1956), constituted prior art.
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HD 99922 is a double star system in the constellation of Crater. It shines with an apparent visual magnitude of 5.77 from a distance of about 450 light years (140 parsecs) away from the Earth. The primary star is an A-type main sequence star; the secondary star is located about 8 arcseconds away. Other designations include HR 4428 and HIP 56078.
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HR 3082 is a double star in the northern circumpolar constellation of Camelopardalis. It is faintly visible to the naked eye with an apparent visual magnitude of 5.39. The system is moving closer to the Sun with a heliocentric radial velocity of +2.7 km/s. It is currently at a distance of around 323 light years, based upon an annual parallax shift of .
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HD 223229 is a suspected variable star in the northern constellation of Andromeda. It is a double star consisting of a magnitude 6.11 primary and a magnitude 8.73 companion. The pair have an angular separation of 0.80″ along a position angle of 250°, as of 2009. The primary is a B-type subgiant star with a stellar classification of B3IV.
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He had been elected a fellow of the Royal Astronomical Society on 10 June 1862. Extracts from his observations at Cambridge 1851-8 appeared in the Astronomische Nachrichten and Monthly Notices. He calculated the orbit of the double star ξ Ursæ Majoris, assigning it a period of 63.14 years, as well as those of Petersen's third (1850) and Brorsen's (1851, iii.) comets.
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Cheng graduated from the Hubei Sports School, entered the Hubei team in 1992, and selected to join the national team in 1998. In 2001, he joined the Qingdao Double Star Badminton Club. He was the men's doubles champion at the 2002 French International partnered with Wang Wei, also the runner-up at the Swiss and Japan Open partnered with Chen Qiqiu.
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It has a stellar classification of K5 and is known to be evolved. The star likely hosts an extrasolar planet, though yet unconfirmed. HD 203857 is listed in the Washington Double Star Catalogue as having five visual companions. It is separated by six arc-minutes from HD 203784, an F-type subgiant, though it is likely they are actually not gravitationally–bound.
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William Herschel listed Delta Equulei as a wide binary. Friedrich Georg Wilhelm von Struve later showed this to be an unrelated optical double star. However his son Otto Wilhelm von Struve while making follow-up observations in 1852 found that while the separation of the optical double continued to increase, Delta Equulei itself appeared elongated. He concluded that it is a much more compact binary.
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The mean separation between them is approximately 10 AU, about the distance between the Sun and Saturn. The binary star has a visual companion, CCDM J13100+1732C, of apparent magnitude 10.2, located 89 arcseconds away along a position angle of 345°.Entry 13100+1732, discoverer code STF1728, components AB-C, The Washington Double Star Catalog , United States Naval Observatory. Accessed on line September 3, 2008.
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Adhafera has about three times the Sun's mass and six times the radius of the Sun. Parallax measurements from the Hipparcos satellite yield an estimated distance to Adhafera of from the Sun. Adhafera forms a double star with an optical companion that has an apparent magnitude of 5.90. Known as 35 Leonis, this star is separated from Adhafera by 325.9 arcseconds along a position angle of 340°.
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Alpha Serpentis (α Serpentis, abbreviated Alpha Ser, α Ser), formally named Unukalhai , is a double star in the head (Serpens Caput) of the equatorial constellation of Serpens. With an apparent visual magnitude of 2.6, this star is the brightest in the constellation and it can be viewed with the naked eye from most of the Earth. Parallax measurements yield an estimated distance of about from the Sun.
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Alpha Lacertae is a blue-white hued main-sequence star of magnitude 3.8, 102 light-years from Earth. It has a spectral type of A1 V and is an optical double star. Beta Lacertae is far dimmer, a yellow giant of magnitude 4.4, 170 light-years from Earth. Roe 47 is a multiple star consisting of five components (magnitudes 5.8, 9.8, 10.1, 9.4, 9.8).
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NGC 6826, the Blinking Planetary Nebula, is a planetary nebula with a magnitude of 8.5, 3200 light-years from Earth. It appears to "blink" in the eyepiece of a telescope because its central star is unusually bright (10th magnitude). When an observer focuses on the star, the nebula appears to fade away. Less than one degree from the Blinking Planetary is the double star 16 Cygni.
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HD 88809 is a star in a double star system in the constellation Antlia. The primary is an orange giant of spectral type K1III. Located around 480 light- years distant, it shines with a luminosity approximately 124 times that of the Sun and has a surface temperature of 4607 K. It has an apparent magnitude of 5.9, while the secondary star has a magnitude of 13.
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Delta Leporis is a yellow giant of magnitude 3.8, 112 light-years from Earth. Epsilon Leporis is an orange giant of magnitude 3.2, 227 light-years from Earth. Kappa Leporis is a double star divisible in medium aperture amateur telescopes, 560 light-years from Earth. The primary is a blue-white star of magnitude 4.4 and the secondary is a star of magnitude 7.4.
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Drawing of Vauban's plan for Strasbourg/Kehl fortifications, circa 1720. Note the multiple channels of the Rhine and its tributaries, and the double star points of the fortifications. The island with the small fortress is Ehrlen. Once the Aulic Council refused Charles's plans, Latour engaged the main French force at Kehl and Charles entrusted to Karl Aloys zu Fürstenberg the command of the siege force at Hüningen.
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The Washington Double Star Catalog lists three visible components for this system. The brightest, component A, is of visual magnitude 4.50. Component B has a magnitude of 7.179, and as of 2000 lies at an angular separation of from A, along a position angle (PA) of 102°. Component C is a magnitude 9.125 star at a separation of from A at a PA of 191°.
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It lies near the ecliptic and thus is subject to occultation by the Moon. One such event was observed September 3, 1991. This system forms a wide double star with an angular separation of along a position angle of 230°, as of 1991. The brighter star, component A, has an apparent magnitude of 4.99 while the fainter secondary, component B, is of magnitude 9.09.
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Beta Pyxidis (Beta Pyx, β Pyxidis, β Pyx) is a double star located in the southern constellation Pyxis. It has an apparent visual magnitude of 3.954, making it the second brightest star in that faint constellation. Based upon parallax measurements, the star is an estimated 420 light-years (128 parsecs) from the Earth. The spectrum matches a bright giant or supergiant star of stellar classification G7Ib-II.
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The five brightest stars are all reddish in hue. Shading the others at apparent magnitude 3.8 is Alpha Apodis, an orange giant that has around 48 times the diameter and 928 times the luminosity of the Sun. Marginally fainter is Gamma Apodis, another ageing giant star. Delta Apodis is a double star, the two components of which are 103 arcseconds apart and visible with the naked eye.
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Since China has started to invest more money into space activities, the Chinese Space Agency has sought international partnerships. ESA is, beside the Russian Space Agency, one of its most important partners. Two space agencies cooperated in the development of the Double Star Mission. In 2017, ESA sent two astronauts to China for two weeks sea survival training with Chinese astronauts in Yantai, Shandong.
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The double star nature of this system was discovered by Robert Hooke in 1664. The two components have an angular separation of 7.606 arcseconds, which can be resolved with a small telescope. The orbital period of the pair is greater than 5000 years. The brighter component, γ² Arietis, is a Lambda Boötis (chemically peculiar) star with a stellar classification of A1p Si and a magnitude of 4.64.
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21 Cancri is a double star in the northern zodiac constellation of Cancer. It is just visible to the naked eye as a dim, red-hued star with an apparent visual magnitude of 6.08. The star is located around 820 light years away from the Sun, based on parallax. It is moving further from the Earth with a heliocentric radial velocity of 35 km/s.
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Mu Geminorum (μ Geminorum, abbreviated Mu Gem, μ Gem), formally named Tejat , is a single star in the northern constellation of Gemini. From parallax measurements obtained during the Hipparcos mission, it is roughly distant from the Sun. Mu Geminorum forms the primary or 'A' component of a double star system designated WDS J06230+2231 along with UCAC2 39641417 (also designated WDS J06230+2231BC), itself a binary pair.
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HD 7853 is a double star in the constellation Andromeda. With an apparent magnitude of 6.46, the stars can barely be seen with the naked eye even on the best of nights. The system is located approximately distant, and the brighter star is an Am star, meaning that it has unusual metallic absorption lines. The spectral type estimates of the primary range between A4 and A9.
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HD 153053 is double star in the southern constellation of Ara. The brighter component is an A-type main sequence star that may be evolving into a subgiant. It has a twelfth magnitude visual companion at an angular separation of 24.7″ along a position angle of 52°. Mostly likely the two are isolated stars that happen to lie near the same line of sight.
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The secondary and tertiary stars are separated by 2 arcseconds; the primary and secondary are separated by 109.1 arcseconds at an angle of 171 degrees. Nu Boötis is an optical double star. The primary is an orange giant of magnitude 5.0 and the secondary is a white star of magnitude 5.0. The primary is 870 light-years away and the secondary is 430 light-years.
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Alpha Caeli (α Cae, α Caeli) is a double star system in the constellation Caelum. Alpha Caeli A is an F-type main sequence star with a stellar classification of F2V and an apparent magnitude of +4.44. It has 1.48 times the mass of the Sun and 1.3 times the solar radius. The projected rotational velocity at the stellar equator is 47.8 km/s.
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3 Geminorum is a blue supergiant star in the constellation Gemini. It is a small amplitude pulsating variable and a close double star, with a mean combined apparent visual magnitude of 5.75. 3 Geminorum was found to be an α Cygni variable in 1998 and given the designation PU Geminorum. It varies by a few tenths of a magnitude with a main period of 3.81 days.
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During 1783 geologist John Michell wrote a letter to Henry Cavendish outlining the expected properties of dark stars, published by The Royal Society in their 1784 volume. Michell calculated that when the escape velocity at the surface of a star was equal to or greater than lightspeed, the generated light would be gravitationally trapped so that the star would not be visible to a distant astronomer. Michell's idea for calculating the number of such "invisible" stars anticipated 20th century astronomers' work: he suggested that since a certain proportion of double-star systems might be expected to contain at least one "dark" star, we could search for and catalogue as many double-star systems as possible, and identify cases where only a single circling star was visible. This would then provide a statistical baseline for calculating the amount of other unseen stellar matter that might exist in addition to the visible stars.
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Rho Scorpii (ρ Scorpii, abbreviated Rho Sco, ρ Sco) is a double star in the constellation of Scorpius. It has an apparent visual magnitude of +3.87, which is bright enough to be seen with the naked eye. Based upon parallax measurements, it is located approximately 472 light years from the Sun. At that distance, the visual magnitude of the system is reduced by 0.07 due to extinction from interstellar dust.
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After Antietam, Key recorded with Eleventh Dream Day's Rick Rizzo on the album Dark Edson Tiger (2000), and they collaborated again on the 2011 album Double Star. Harris went on to record with Yo La Tengo and The Special Pillow. Madell went on to drum for Codeine and Retsin. In 1996, Key performed with Yo la Tengo as The Factory's house band in the film I Shot Andy Warhol.
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This dust has a mean temperature of 300 K and is orbiting at a radius of 1.7 AU, compared to a projected linear separation of 0.23 AU for the components. The Washington Double Star Catalog lists two additional visual components. Component B is a magnitude 12.6 star at an angular separation of 77 arcseconds from the primary system. Component C is magnitude 13.0 and is located 71 arcseconds away.
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Delta¹ Tauri (δ¹ Tauri, abbreviated Delta¹ Tau, δ¹ Tau) is a double star in the zodiac constellation of Taurus. Based upon an annual parallax shift of 20.96 mas as seen from Earth, it is located roughly 156 light-years distant from the Sun. The system is faintly visible to the naked eye with a combined apparent visual magnitude of +3.772. It is considered a member of the Hyades cluster.
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NGC 1241 forms a pair with NGC 1242, which lies at an angular separation of 1.6 arcminutes. NGC 1243 lies 3.1 arcminutes away, but it has been identified as a double star in our galaxy. According to Garcia et al. the pair of galaxies is part of a galaxy group known as LGG 84, which also includes the galaxies NGC 1247, MCG -02-09-006, and Markarian 1071.
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A double star, it has a companion of magnitude 13; the two are separated by 11 arcseconds. Beta Pictoris Comparison Located about 1298 light-years from Earth, Delta Pictoris is an eclipsing binary of the Beta Lyrae type. Composed of two blue stars of spectral types B3III and O9V, the system has a period of 1.67 days, and is observed to dip from apparent magnitude 4.65 to 4.9.
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Zeta Reticuli, Latinized from ζ Reticuli, is a wide binary star system in the southern constellation of Reticulum. From the southern hemisphere the pair can be seen with the naked eye as a double star in very dark skies. Based upon parallax measurements, this system is located at a distance of about from Earth. Both stars are solar analogs that have characteristics similar to those of the Sun.
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Iota Cancri is a wide double star. The primary is a yellow-hued G-type bright giant star of magnitude 4.0, located 330 ± 20 light-years from Earth. It spent much of its stellar life as a B-type main sequence star before expanding and cooling to its current state as it spent its core hydrogen. The secondary is a white main sequence star of spectral type A3V and magnitude 6.57.
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Another star visible to the naked eye is γ Capricorni, sometimes called Nashira ("bringing good tidings"); it is a white-hued giant star of magnitude 3.7, 139 light-years from Earth. π Capricorni is a double star with a blue-white hued primary of magnitude 5.1 and a white-hued secondary of magnitude 8.3. It is 670 light-years from Earth and the components are distinguishable in a small telescope.
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2 Equulei is a double star system in the constellation of Equuleus. The primary component of the 2 Equ pair is an F-type main sequence star. As of 2015, the secondary had an angular separation of 2.90 arc seconds along a position angle of 213° from the primary. They form a common proper motion pair, two stars at approximately the same distance and moving in the same direction.
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He succeeded his father as director of Harvard College Observatory from 1859 until his death. His cousin was Edward Singleton Holden, first director of Lick Observatory. Bond took the first photograph of a star in 1850 (Vega) and of a double star in 1857 (Mizar); suggested photography could be used to measure a star's magnitude; and discovered numerous comets and calculated their orbits. Bond also studied Saturn and the Orion Nebula.
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41 Aquarii is a double star in the equatorial constellation of Aquarius. 41 Aquarii is its Flamsteed designation. It is visible to the naked eye as a dim, orange-hued point of light with a combined apparent visual magnitude of 5.354. The pair are located at a distance of around from the Sun based on parallax, but are drifting closer with a radial velocity of –25 km/s.
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Nu Draconis (also known as ν Dra, ν Draconis, or traditionally as Kuma ) is a double star in the constellation Draco. The respective components are designated ν1 Draconis and ν2 Draconis. The second component is a spectroscopic binary star system. This star, along with β Dra (Rastaban), γ Dra (Eltanin), μ Dra (Erakis) and ξ Dra (Grumium) were Al ʽAwāïd, "the Mother Camels", which was later known as the Quinque Dromedarii.
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The Aitken Double Star Catalogue, or ADS, is a star catalogue of double stars. It was compiled by Robert Grant Aitken and published in 1932 in two volumes, under the name New general catalogue of double stars within 120° of the North Pole. It contains measurements of 17,180 double stars north of declination −30°. Entries in this catalogue are generally referred to by an index number prefixed with the letters ADS.
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All known doubles were periodically re-measured to determine their orbits. With Thiele, Innes formulated a simplified method of specifying double star orbits. These orbital parameters when combined with other measurements, such as radial velocity allow the mass of each star of the binary pair to be determined. Mass, combined with luminosity and temperature or spectral type, is a fundamental parameter needed in theories of stellar structure and stellar evolution.
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Theta Sagittae (θ Sagittae) is a double star in the northern constellation of Sagitta. With a combined apparent visual magnitude of +6, it is near the limit of stars that can be seen with the naked eye. According to the Bortle scale the star is visible in dark suburban/rural skies. Based upon an annual parallax shift of as seen from Earth, it is located roughly from the Sun.
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The binary pair consists of two stars separated by . The primary, component A, is an F-type main sequence star with a stellar classification of F3V. This star is about two billion years old with 52% more mass than the Sun. It forms a double star with a magnitude 8.85 companion, which is located at an angular separation of along a position angle of 331.1°, as of 2011.
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Eta Antliae (η Ant, η Antliae) is the Bayer designation for a double star in the southern constellation of Antlia. The brighter component has an apparent visual magnitude of 5.222, making it visible to the naked eye. Parallax measurements of the system yield a distance estimate of from Earth. The main component has a stellar classification of F1 V, which indicates that it is an F-type main sequence star.
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V, orbiting about 250 AU from the primary. It has a Gaia Data Release 2 parallax of , corresponding to a distance of . An 11th-magnitude star is listed in double-star catalogues as component C of the multiple system. It was away from component A in 2002, although the separation is rapidly increasing as it is a distant background object with a very different proper motion to the other two stars.
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The binary was measured by William Herschel in 1779 however Christian Mayer, listed an earlier observation in his first double-star catalog in 1784 so its true discoverer is not clear. The two stars have an orbital period of about 587 years. The semimajor axis is 3.8 arcseconds and they have an orbital eccentricity of 0.40. The orbital plane is inclined by 138.2° to the line of sight.
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Rho Herculis (ρ Her, ρ Herculis) is a double star in the constellation of Hercules. The apparent magnitudes of the components are 4.510 and 5.398, respectively. Parallax measurements published in Gaia Data Release 2 put the system at some 360-390 light-years (111-121 parsecs) away. The two stars of Rho Herculis are separated by four arcseconds, and are known as Rho Herculis A and B, respectively.
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Hubble was used via the FGS sensors to detect the motion of star caused by an exoplanet orbiting it. The effect on the Star Gliese 876's by companion Gliese 876b was measured. That star is known as a red dwarf about 15 light-years away from Earth.Gliese 876 FGS was used to study Double-star systems (aka Binary star systems) and to measure distances to astronomical bodies.
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The two stars orbit each other every ten days and are a mere 0.1 AU apart. This system is the closest in the constellation to the Earth. Only of magnitude 5.25, 7 Trianguli is much further away at around 280 light-years distant from Earth. Iota Trianguli is a double star whose components can be separated by medium-sized telescopes into a strong yellow and a contrasting pale blue star.
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There is a faint star that appears close enough to β Tauri for astronomers to consider it a double star. Its visual companion, known as BD+28 795B, has a position angle of 239 degrees and is separated from the main star by 33.4 arcseconds. Six closer and even fainter stars have been detected during a search for brown dwarf and planetary companions, but all are considered to be background objects.
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Drawing of Vauban's plan for Strasbourg/Kehl fortifications, circa 1720. Note the multiple channels of the Rhine and its tributaries, and the double star points of the fortifications. Everything went according to the French plan, at least for the first six weeks. On 4 June 1796, 11,000 soldiers of the Army of the Sambre-et-Meuse, commanded by François Lefebvre, pushed back a 6,500-man Austrian force at Altenkirchen.
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In 1951, component A was resolved into a double separated by only 0.15", with an estimated orbital period of 250 years. The Washington Double Star catalogue lists the pair as magnitude 4.89 Aa and magnitude 5.33 Ab, but the CCDM designates the components as A and P. A 10th magnitude component E was discovered in 2010. It is less than 1" away from the 4th magnitude main component.
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It lies half a degree away from S Persei, another red supergiant Double Cluster member. T Per is a semiregular variable star, whose brightness varies from magnitude 8.34 to 9.7 over a period of 2,430 days. Unlike many red supergiants, it does not appear to have a long secondary period. The Washington Double Star Catalog lists T Persei as having a 9th magnitude companion 0.1 arc-seconds away.
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Epsilon Reticuli (Epsilon Ret, ε Reticuli, ε Ret) is a double star approximately 59 light-years away in the constellation of Reticulum. The primary component is an orange subgiant, while the secondary is a white dwarf. The two stars share a common motion through space and hence most likely form a binary star system. The brighter star should be easily visible without optical aid under dark skies in the southern hemisphere.
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Nu Ursae Majoris (ν Ursae Majoris, abbreviated Nu UMa, ν UMa), formally named Alula Borealis , is a double star in the northern circumpolar constellation of Ursa Major. At an apparent visual magnitude of +3.490, it is bright enough to be seen with the naked eye. Based upon parallax measurements, the distance to ν Ursae Majoris is about . This is a giant star with a stellar classification of K3 III.
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HD 203857 is a double star in the constellation Cygnus. It is near the lower limit of visibility to the naked eye, having a combined apparent visual magnitude of 6.46. The distance to the primary component is approsimatly 1,230 light years based on parallax, and it has an absolute magnitude of −0.75. The star is drifting closer to the Sun with a radial velocity of −6.3 km/s.
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Accessed on line 9 June 2013.Notes file for the WDS , WDS Catalog United States Naval Observatory. Accessed on line 9 June 2013.References and discoverer codes, The Washington Double Star Catalog , United States Naval Observatory. Accessed on line 9 June 2013. These double star observations were all made roughly between December 1827 and December 1828, being observed through his homemade 9-foot 23 cm (9-inch) speculum Newtonian reflector, or by measuring the separated distances and position angles of selected double stars using the small equatorial mounted refracting telescope. Most of these pairs have proved to be uninteresting to astronomers, and many of the double stars selected were too wide for the indication of orbital motion as binary stars. It seems these observations were made when the atmospheric conditions were quite unsuitable for looking at deep sky objects, either being made under unsteady astronomical seeing or when the sky was illuminated by the bright moon.
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During Southwood's tenure, ESA expanded its cooperation with other space agencies. ESA worked with China on the Double Star and Chang’e missions, and with India on Chandrayaan-1. Collaborative missions initiated with the US included the James Webb Space Telescope, where Southwood secured the flight of two predominantly European instruments (MIRI and NirSpec) and arranged a European launch on Ariane 5. In 2008, Southwood became ESA's first Director of Science and Robotic Exploration.
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Elias 2-27 (2MASS J16264502-2423077) is a YSO star with a protoplanetary disc around it, located in the Ophiuchus Molecular Cloud (ρ Oph Cld, 5 Oph Cld, Ophiuchus Dark Cloud), a star-forming region in the Ophiuchus constellation, some away. This star system became the first ever observed with density waves in the disc, giving it a spiral structure. Elias 2-27 is located near the double star Rho Ophiuchi (5 Ophiuchi).
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HD 211415 is a double star in the constellation Grus. With an apparent visual magnitude of 5.33, it is visible to the naked eye. The annual parallax shift is 72.54 mas, which yields a distance estimate of 45 light years. It has a relatively high proper motion, traversing the celestial sphere at the rate of 93.4 mas per year, and is moving closer to the Sun with a radial velocity of −13 km/s.
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Supernovae can result from the death of an extremely massive star, many times heavier than the Sun. At the end of the life of this massive star, a non-fusible iron core is formed from fusion ashes. This iron core is pushed towards the Chandrasekhar limit till it surpasses it and therefore collapses. A supernova may also result from mass transfer onto a white dwarf from a star companion in a double star system.
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Much smaller than the primary, the white dwarf cannot be seen as a separate object, even by the Hubble Space Telescope. Gamma Crateris is a double star, resolvable in small amateur telescopes. The primary is a white main sequence star of spectral type A7V, that is an estimated 1.81 times as massive as the Sun, while the secondary—of magnitude 9.6—has 75% the Sun's mass, and is likely an orange dwarf.
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Iconaster longimanus, the icon star or double star, is a species of starfish in the family Goniasteridae. It is found in the west and central Indo-Pacific Ocean. The genus name comes from the Greek eikon, meaning portrait or image and possibly referring to the way the marginal plates frame the disc, and aster, meaning star. The specific name comes from the Latin longus manus and refers to the long, slender arms.
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The double star Zeta Reticuli is located in the western part of the small Reticulum constellation, about 25′ from the constellation's border with Horologium. In dark southern skies, the two stars can be viewed separately with the naked eye, or with a pair of binoculars. ζ1 Reticuli has an apparent magnitude of 5.52, placing it on the border between 5th and 6th magnitude stars. ζ2 Reticuli is slightly brighter at magnitude 5.22.
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Since 1700, two calendar variants were in force in the German Reich: the Gregorian Calendar in the catholic, the Verbesserter Reichskalender (improved Reich calendar) in the Protestant regions, however the latter differed from the former solely in respect of calculation of the date of Easter. The crater Kirch on the Moon and the asteroid 6841 Gottfriedkirch are named after him. Kirch studied the double star Mizar. He died at Berlin at the age of seventy.
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To small telescopes, Theta Muscae appears as a double star, with a blue-cream brighter star and an O9III companion of magnitude 7.3 some 5.3 arcseconds away. The primary θ Muscae A is a massive triple star system. The companion θ Muscae B is not part of the triple system but an optical double which happens to be along the same line of sight. It is a luminous O class giant star.
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Eta Boötis (η Boötis, abbreviated Eta Boo, η Boo) is a binary star in the constellation of Boötes. Based on parallax measurements obtained during the Hipparcos mission, it is approximately 37 light-years (11 parsecs) distant from the Sun. Since 1943, the spectrum of this star has served as one of the stable anchor points by which other stars are classified. It forms a double star with the star BD+19 2726.
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This is a double star and possible binary system. The primary component has a stellar classification of G2 Ib/II, which places it on the borderline between the bright giant and lower luminosity supergiant stars. It has passed the first dredge-up and may be undergoind Cepheid-like pulsations. With more than four times the mass of the Sun, this is an evolved star that has reached its current stage after only 135 million years.
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Upsilon Librae (υ Lib, υ Librae) is the Bayer designation for a double star in the zodiac constellation Libra. With an apparent visual magnitude of 3.628, it is visible to the naked eye. The distance to this star, based upon an annual parallax shift of 14.58, is around 224 light years. It has a magnitude 10.8 companion at an angular separation of 2.0 arc seconds along a position angle of 151°, as of 2002.
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HR 4177, also called t² Carinae (t² Car), is a double star in the southern constellation of Carina. It is faintly visible to the naked eye with a combined apparent visual magnitude of +4.77. The two components are HD 92397 and HD 92398. The primary component is located at a distance of approximately 1,600 light years from the Sun based on parallax, and is drifting further away with a radial velocity of +11 km/s.
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In 1906, he published the Burnham Double Star Catalogue, containing 13,665 pairs of stars. The quality of Burnham's work opened the doors of observatories for him and he had access to more powerful instruments at Lick, Yerkes, and other observatories. He is credited with having discovered 1,340 binary stars. Burnham discovered the first example of, what would be called a half century later, a Herbig–Haro object, called Burnham's Nebula (now labeled as HH 255).
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Beta Hydrae (Beta Hya, β Hydrae, β Hya) is a double star in the constellation of Hydra. Its overall apparent visual magnitude varies by 0.04 magnitudes with a period of 2.344 days, and is approximately 4.27 at maximum brightness.bet Hya, database entry, The combined table of GCVS Vols I-III and NL 67-78 with improved coordinates, General Catalogue of Variable Stars, Sternberg Astronomical Institute, Moscow, Russia. Accessed on line September 23, 2008.
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The components of multiple stars can be specified by appending the suffixes A, B, C, etc., to the system's designation. Suffixes such as AB may be used to denote the pair consisting of A and B. The sequence of letters B, C, etc. may be assigned in order of separation from the component A.Format, The Washington Double Star Catalog , Brian D. Mason, Gary L. Wycoff, and William I. Hartkopf, Astrometry Department, United States Naval Observatory.
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She took pictures of planets, such as Jupiter and Saturn, as well as their moons, and she studied nebulae, double stars, and solar eclipses. Mitchell then developed theories around her observations, such as the revolution of one star around another in double star formations and the influence of distance and chemical composition in star color variation. Mitchell often involved her students with her astronomical observations in both the field and the Vassar College Observatory.
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This emission can be characterized by heat radiated from dust at a temperature of 85 K, which corresponds to an orbital radius of 88 Astronomical Units, or 88 times the distance of the Earth from the Sun. For comparison, the region of the remote Kuiper belt in the Solar System extends from 30–50 AU. The Washington Double Star Catalog lists a 12th magnitude companion away. It is an unrelated background object.
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Dusty ring around double star IRAS 08544-4431. The next brightest star is Delta Velorum or Alsephina, also a multiple star system and one of the brightest eclipsing binaries in the sky. Together with Kappa Velorum or Markeb, Iota Carinae or Aspidiske and Epsilon Carinae or Avior, it forms the diamond-shaped asterism known as the False Cross—so called because it is sometimes mistaken for the Southern Cross, causing errors in astronavigation.
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With a diameter 130 times that of our Sun, it would almost reach the orbit of Venus if placed at the centre of the Solar System. The proper name Atria is a contraction of its Bayer designation. Beta Trianguli Australis is a double star, the primary being a F-type main-sequence star with a stellar classification of F1V, and an apparent magnitude of 2.85. Lying only away, it has an absolute magnitude of 2.38.
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MWC 349 is a resolved double star, with its components separated by 2.4 arc seconds. The primary, MWC 349A, is a B[e] star, where the B is the spectral type and the [e] denotes forbidden emission lines. Its spectrum lacks absorption features and is variable but has been classified as B0-1.5 with a supergiant luminosity class. The secondary, MWC 349B, is a giant star with a spectral type of B0III.
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An easily split visual target, Mizar was the first telescopic binary discovered, most probably by Benedetto Castelli who in 1617 asked Galileo Galilei to observe it. Galileo then produced a detailed record of the double star. Later, around 1650, Riccioli wrote of Mizar appearing as a double. The secondary star (Mizar B) comes within 380 AU of the primary (Mizar A) and the two take thousands of years to revolve around each other.
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HD 221776 is a double star in the northern constellation of Andromeda. With an apparent visual magnitude of 6.18,, it is viewable by the naked eye user very favourable conditions. The most luminous component has a spectral classification K5III, meaning that it's an orange giant star that has evolved off the main sequence. An infrared excess has been detected around this star, indicating the star is associated with a cloud of dust particles.
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KU Hydrae is a binary star in the constellation Hydra. The primary star is an Alpha2 Canum Venaticorum variable with its apparent magnitude varying from 0.05 magnitudes over a period of 33.97 days. This star was discovered to be a visual binary star by Robert Grant Aitken in 1906 and was given the double star designation A 1342. Additional measurements of the position angle and angular separation showed a rapid orbital motion.
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HD 150136 is listed in the Washington Double Star Catalog as having seven visual components within 30 arc seconds. Component A is a close triple system containing three massive class O main sequence stars. The brightest companion is catalogued individually as HD 150135 as well as component C of the multiple system, separated by only 10 arc-seconds. It is another O class spectroscopic binary and also a member of NGC 5193.
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Dunlop's other major observational work was of 256 southern double stars or "pairs" below the declination of about 30° South. These were listed in Approximate Places of Double Stars in the Southern Hemisphere, observed at Paramatta in New South Wales, published in 1829. Many of these pairs were actual new discoveries, though the most northerly of them had been earlier discoveries made by other observers. The Washington Double Star Catalog , WDS Catalog United States Naval Observatory.
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The Xichang Satellite Launch Center (XSLC), also known as the Xichang Space Center, is a spaceport of China. It is located in Zeyuan Town (), approximately northwest of Xichang, Liangshan Yi Autonomous Prefecture in Sichuan. The facility became operational in 1984 and is used to launch numerous civil, scientific, and military payloads annually. It is notable as the site of Sino-European space cooperation, with the launch of the first of two Double Star scientific satellites in December 2003.
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ADS 48 is a multiple star system in the constellation of Andromeda consisting of 7 stars. The components, in order from A to G, have apparent visual magnitudes of 8.826, 8.995, 13.30, 12.53, 11.68, 9.949, and 13.00. ADS 48A and ADS 48B are in orbital motion around each other while ADS 48F is a common proper motion companion not gravitationally bound to the pair. The others are unassociated background stars, and component C could be a double star itself.
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78 Pegasi is a binary star system in the northern constellation of Pegasus. It is visible to the naked eye as a faint, orange-hued point of light with an apparent visual magnitude of 4.93. The system is located approximately 224 light years from the Sun based on parallax, but is drifting closer with a radial velocity of −8 km/s. The double-star nature of this system was discovered by A. G. Clark in 1862.
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Despite this some discoveries include the Moons of Mars, a fifth Moon of Jupiter, and many double star discoveries including Sirius (the Dog star). Refactors were often used for positional astronomy, besides from the other uses in photography and terrestrial viewing. Singlets The Galilean moons and many other moons of the solar system, were discovered with single-element objectives and aerial telescopes. Galileo Galilei's discovered the Galilean satellites of Jupiter in 1610 with a refracting telescope.
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Map of Paz, the continent group in which the Dray Prescot series is set. The series is set on the fictional world of Kregen, a planet of the Antares star system in the constellation of Scorpio. Antares is envisioned as a double star system consisting of a large red giant (Antares A) and a smaller green star (Antares B). Antares B is in reality blue, though often described as green, probably owing to a contrast effect.James Kaler, "Antares".
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Carter's "Demon Trinity" (Ghatanothoa, Ythogtha, and Zoth-Ommog) were spawned on a planet near the double star Xoth. They are the progeny of a mating between CthulhuCthulhu and Ghatanathoa were originally the creations of Lovecraft, appearing in "The Call of Cthulhu" (1928) and "Out of the Aeons" (1935), respectively. While Lovecraft never established a connection between these beings, Robert M. Price, believes that Ghatanothoa is essentially a revised version of Cthulhu. () and the quasi- female entity Idh-yaa.
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16 Cygni Bb or HD 186427 b is an extrasolar planet approximately 69 light- years away in the constellation of Cygnus. The planet was discovered orbiting the Sun-like star 16 Cygni B, one of two solar-mass () components of the triple star system 16 Cygni in 1996. It orbits its star once every 799 days and was the first eccentric Jupiter and planet in a double star system to be discovered. The planet is abundant in Lithium.
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The brightest member of the σ Orionis system appears as a late O class star, but is actually made up of three stars. The inner pair complete a highly eccentric orbit every 143 days, while the outer star completes its near-circular orbit once every 157 years. It has not yet completed a full orbit since it was first discovered to be a double star. All three are very young main sequence stars with masses between .
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In October of the same year he earned a PhD, under the advisory of Klinkerfues, with a thesis titled "Untersuchungen über die Bahn des Doppelsterns 70 p Ophiuchi" ("Studies on the orbit of the double star 70 p Ophiuchi"). In the winter of 1867/1868 Schur moved to the University of Berlin, where he attended lectures in astronomy by Arthur von Auwers and Wilhelm Foerster and in physics by Heinrich Wilhelm Dove, Johann Christian Poggendorff, and Georg Quincke.
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To cope with the sterile habitat, the human colonists abuse drugs such as "Can-D" and "Chew-Z". Dick previously published a shorter version of the story in 1963, called All We Marsmen. Like Heinlein's Double Star, All We Marsmen was conceived at a time in US history when many marginalized people were fighting especially vehemently for more civil rights. US President Lyndon B. Johnson signed the Civil Rights Act of 1964 into law on 2 July 1964.
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Ludwig Ignaz Schupmann (23 January 1851 in Geseke (Westphalia), Germany – 2 October 1920 also in Geseke) was a German professor of architecture and an optical designer. He is principally remembered today for his Medial and Brachymedial telescopes, types of catadioptric reflecting-refracting telescopes with Mangin mirrors that eliminate chromatic aberrations while using common optical glasses. Used in early lunar studies, they are used now in double-star work. The asteroid 5779 Schupmann is named in his honour.
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HD 19789 is a double star in the northern constellation of Aries. The primary component has an orange hue and is barely visible to the naked eye with an apparent visual magnitude of 6.11. it is located at a distance of approximately 390 light years from the Sun based on parallax, and is drifting further away with a radial velocity of +8 km/s. The star is located near the ecliptic and thus is subject to lunar occultations.
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ESO Supernova building. The visitor centre was designed by the architects Bernhardt + Partner, that already designed the Haus der Astronomie, a centre for astronomy education and outreach. The design of the ESO Supernova resembles that of a close double-star system with one star transferring mass to its companion. This set-up will ultimately lead to the heavier component exploding as a supernova, briefly becoming as bright as the light of all the stars in the Milky Way combined.
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Lambda1 Sculptoris, Latinized from λ1 Sculptoris, is a double star system in the southern constellation of Sculptor. It is close to the lower limit of visibility to the naked eye, with a combined apparent visual magnitude of +6.05. Based upon an annual parallax shift of 6.89 mas as measured from Earth, it is located roughly 470 light years from the Sun. At that distance, the visual magnitude is diminished by an extinction factor of 0.026 due to interstellar dust.
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Xi2 Lupi (ξ2 Lup, ξ2 Lupi) is a member of a double star with Xi1 Lupi in the southern constellation of Lupus. As of 2004, the pair had an angular separation of 10.254 arc seconds along a position angle of 49.21°. Xi2 Lupi is visible to the naked eye with an apparent visual magnitude of 5.55. Based upon an annual parallax shift of 21.71 mas as seen from Earth, it is located roughly 150 light years from the Sun.
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Alpha Aquarii (α Aquarii, abbreviated Alpha Aqr, α Aqr), officially named Sadalmelik , is a single star in the constellation of Aquarius. The apparent visual magnitude of 2.94 makes this the second-brightest star in Aquarius. Based upon parallax measurements made during the Hipparcos mission, it is located at a distance of roughly from the Sun. It forms the primary or 'A' component of a double star designated WDS J22058-0019 (the secondary or 'B' component is UCAC2 31789179).
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The two components are yellow main sequence stars. The brighter component (designated Xi Ursae Majoris A), has a mean apparent magnitude of +4.41. The companion star (Xi Ursae Majoris B) has an apparent magnitude of +4.87. The orbital period of the two stars is 59.84 years, and they are currently separated by 1.2 arcseconds, or at least 10 AU. Orbit of Xi Ursae Majoris Each component of this double star is itself a single-lined spectroscopic binary.
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Beta Trianguli Australis, Latinized from β Trianguli Australis, is a double star in the southern circumpolar constellation of Triangulum Australe. It is approximately from Earth and has an apparent visual magnitude of +2.85. This star has a relatively high rate of proper motion across the celestial sphere. It is a F-type main-sequence star with a stellar classification of F1 V. Beta TrA has a 14th magnitude optical companion at an angular separation of 155 arcseconds.
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12 Camelopardalis is a binary star in the northern circumpolar constellation of Camelopardalis, located 700 light years away from the Sun as determined from parallax measurements. It forms a double star with 11 Camelopardalis, which is only 3 arcminutes away. The system has the variable star designation BM Camelopardalis; 12 Camelopardalis is the Flamsteed designation. It is just visible to the naked eye, appearing as a dim, orange-hued star with an apparent visual magnitude of 6.08.
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The Lambda Orionis Cluster (also known as the Collinder 69) is an open star cluster located north-west of the star Betelgeuse in the constellation of Orion. It is about five million years old and roughly away from the Sun. Included within the cluster is a double star named Meissa. With the rest of Orion, it is visible from the middle of August in the morning sky, to late April before Orion becomes too close to the Sun to be seen well.
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The seven stars that make up the constellation's distinctive crown-shaped pattern are all 4th-magnitude stars except for the brightest of them, Alpha Coronae Borealis. The other six stars are Theta, Beta, Gamma, Delta, Epsilon and Iota Coronae Borealis. The German cartographer Johann Bayer gave twenty stars in Corona Borealis Bayer designations from Alpha to Upsilon in his 1603 star atlas Uranometria. Zeta Coronae Borealis was noted to be a double star by later astronomers and its components designated Zeta1 and Zeta2.
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Delta1 Chamaeleontis, Latinized from δ1 Chamaeleontis, is a close double star located in the constellation Chamaeleon. It has a combined apparent visual magnitude of 5.47, which is just bright enough for the star to be faintly seen on a dark rural night. With an annual parallax shift of 9.36 mas, it is located around 350 light years from the Sun. This pair is one of two stars named Delta Chamaeleontis, the other being the slightly brighter Delta2 Chamaeleontis located about 6 arcminutes away.
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The two stars are distinguishable by the naked eye, and both are themselves multiple stars. α1 Capricorni is accompanied by a star of magnitude 9.2; α2 Capricornus is accompanied by a star of magnitude 11.0; this faint star is itself a binary star with two components of magnitude 11\. Also called Algedi or Giedi, the traditional names of α Capricorni come from the Arabic word for "the kid", which references the constellation's mythology. β Capricorni is a double star also known as Dabih.
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RR Caeli is a double star in the constellation Caelum. It is approximately 66 light years from Earth. It was first noted to be a high-proper motion star in 1955 by Jacob Luyten, and given the name LFT 349. Discovered to be an eclipsing binary in 1979, it has a baseline magnitude of 14.36, dimming markedly every 7.2 hours for an interval of around 10 minutes, due to the total eclipse of the brighter star by the fainter one.
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For instance, the anthropologist Walter Van Beek, who studied the Dogon after Griaule and Dieterlen, found no evidence that the Dogon considered Sirius to be a double star and/or that astronomy was particularly important in their belief system.Holberg, Jay B. Sirius Springer 2007 p176 Others, such as Marcel Griaule's daughter Geneviève Calame-Griaule and an anthropologist, Luc de Heusch, came to criticize Van Beek's dismissal as "political" and riddled with "unchecked speculation", demonstrating a general ignorance of Dogon esoteric tradition.
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Delta Apodis (δ Aps, δ Apodis) is the Bayer designation for a double star in the southern constellation of Apus. The brighter star, δ¹ Apodis, is a M-type red giant and has an apparent magnitude that varies from magnitude +4.66 to +4.87. It is classified as a semiregular variable with pulsations of multiple periods of 68.0, 94.9 and 101.7 days. At an angular separation of 102.9 arcseconds is δ² Apodis, an orange K-type giant with an apparent magnitude of +5.27.
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Mu Bootis (Alkalurops) as seen in a small telescope Mu Boötis, Latinized from μ Boötis, consists of a pair of double stars in the northern constellation of Boötes. The primary pair, components Aa, are designated μ1 Boötis and have an angular separation of 0.08″. The secondary, consisting of components BC, is designated μ2 Boötis and they have a separation of 2.2″. The two double star systems are separated by 107″, with matching parallaxes and proper motions, suggesting they form a system.
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Following the success of the Double Star mission, the ESA and CAS decided to jointly select, design, implement, launch and exploit the results of a space mission together for the first time. After initial workshops, a call for proposals was announced in January 2015. After a joint peer review of mission proposals, SMILE was selected as the top candidate out of 13 proposed. The SMILE mission proposal was jointly led by the University College London and the Chinese National Space Science Center.
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He was not able to measure its distance accurately with his 9-inch refractor or the short focus Franklin-Adams astrograph. The definitive distance was measured by Harold Lee Alden at the Yale observatory station in Johannesburg which was equipped with a long focus camera designed for stellar parallax work. Alden’s more precise measurements confirmed Proxima to be the closest star to the sun. No closer star has been found to date. Visual double star observation was Innes’ main contribution to astronomy.
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The seventh companion published for Capella, component H, is physically associated with the bright primary star. It is a red dwarf separated from the pair of G-type giants by a distance of around 10,000 AU. It has its own close companion, an even fainter red dwarf that was 1.8" away when it was discovered in 1935. Eighty years later the separation had increased to 3.5", sufficient to allow tentative orbital parameters to be derived. It is component L in double star catalogues.
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Delta Arae, Latinized from δ Arae, is the Bayer designation for a double star in the southern constellation Ara. It has an apparent visual magnitude of 3.62 and is visible to the naked eye. Based upon an annual parallax of 16.48 mas, it is about distant from the Earth. Delta Arae is massive B-type main sequence star with a stellar classification of B8 Vn. The 'n' suffix indicates the absorption lines are spread out broadly because the star is spinning rapidly.
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HD 171301 and BD+30°3223B are two components of a double star in the constellation Lyra, approximately 370 light years away from Earth. The brighter of the pair, 5th magnitude HD 171301, is a subgiant star with the spectral type B8IV. It therefore possesses a surface temperature of 11,000 to 25,000 kelvins and is brighter, larger, and at least twice as hot as our Sun. Its companion, BD+30°3223B, is a 13th magnitude star of an unknown spectral type.
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It is now so entered in the IAU Catalog of Star Names. 20 Tauri is the star's Flamsteed designation. Although it is about the 15th brightest star in Taurus, Maia does not have a Bayer designation, but does have the Bright Star Catalogue designation HR 1149 and the Henry Draper Catalogue designation HD 23408. It has been listed as double star WDS J03458+2422; one companion is a 14th magnitude star nearly away that is probably an unrelated background object.
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At the conclusion of his double star work in 1905, he had discovered and measured 1,327 close binaries. For this work, he was awarded the Lalande Medal in 1906, which he shared with Robert Grant Aitken. He was born at Mendon, Ohio, August 10, 1862, son of John Milton and Mary Catherine (Severns) Hussey. After graduating with a BS in civil engineering from the University of Michigan in 1889, he served as assistant in the Nautical Almanac Office of Washington.
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NGC 346 is a young open cluster of stars with associated nebula located in the Small Magellanic Cloud (SMC) that appears in the southern constellation of Tucana. It was discovered August 1, 1826 by Scottish astronomer James Dunlop. J. L. E. Dreyer described it as, "bright, large, very irregular figure, much brighter middle similar to double star, mottled but not resolved". On the outskirts of the cluster is the multiple star system HD 5980, one of the brightest stars in the SMC.
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Zeta Ceti (ζ Ceti, abbreviated Zeta Cet, ζ Cet) is a binary star in the equatorial constellation of Cetus. It has a combined apparent visual magnitude of 3.74, which is bright enough to be seen with the naked eye. Based upon parallax measurements taken during the Hipparcos mission, it is approximately 235 light-years from the Sun. Zeta Ceti is the primary or 'A' component of a double star system designated WDS J01515-1020 (the secondary or 'B' component is HD 11366).
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At least 1 in 18 stars brighter than 9.0 magnitude in the northern half of the sky are known to be double stars visible with a telescope.The Binary Stars, Robert Grant Aitken, New York: Dover, 1964, p. 260. The unrelated categories of optical doubles and true binaries are lumped together for historical and practical reasons. When Mizar was found to be a binary, it was quite difficult to determine whether a double star was a binary system or only an optical double.
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The binary system described above has an optical visual companion, discovered by William Herschel on July 21, 1781.See p.140, entry 32 in Designated as ADS 94 B in the Aitken Double Star Catalogue, it is a G-type star with an apparent visual magnitude of approximately 10.8. Although by coincidence it appears near to the other two stars in the sky, it's much more distant from Earth; the parallax observed by Gaia place this star more than 1,300 light years away.
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It includes a naked eye double star, Theta Tauri (the proper name of Theta2 Tauri is Chakumuy), with a separation of 5.6 arcminutes. In the northeastern quadrant of the Taurus constellation lie the Pleiades (M45), one of the best known open clusters, easily visible to the naked eye. The seven most prominent stars in this cluster are at least visual magnitude six, and so the cluster is also named the "Seven Sisters". However, many more stars are visible with even a modest telescope.
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Mizar is a second-magnitude star in the handle of the Big Dipper asterism in the constellation of Ursa Major. It has the Bayer designation ζ Ursae Majoris (Latinised as Zeta Ursae Majoris). It forms a well-known naked eye double star with the fainter star Alcor, and is itself a quadruple star system. The whole system lies about 83 light-years away from the Sun, as measured by the Hipparcos astrometry satellite, and is part of the Ursa Major Moving Group.
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Xi1 Lupi (ξ1 Lup, ξ1 Lupi) is a probable binary star in the southern constellation of Lupus. It is faintly visible to the naked eye with an apparent visual magnitude of 5.1, and forms a visual double star with Xi2 Lupi. Based upon an annual parallax shift of 23.60 mas as seen from Earth, it is located around 140 light years from the Sun. It is a member of the Upper Scorpius sub-group of the nearby Sco OB2 association.
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19 Tauri is a double star in the constellation of Taurus and a member of the Pleiades open star cluster (M45). It consists of a binary pair designated 19 Tauri A together with a single star visual companion, 19 Tauri B. 'A's' two components are themselves designated 19 Tauri Aa (officially named Taygeta , the traditional name for the entire system) and Ab. Based on parallax measurements obtained during the Hipparcos mission, 19 Tauri A is approximately 440 light-years from the Sun.
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Pleione is known to be a speckle binary, although its orbital parameters have yet to be fully established. In 1996 a group of Japanese and French astronomers discovered that Pleione is a single-lined spectroscopic binary with an orbital period of 218.0 days and a large eccentricity of 0.6. The Washington Double Star Catalogue lists an angular separation between the two components of 0.2 arcseconds—an angle which equates to a distance of about 24 AU, assuming a distance of 120 parsecs.
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V810 Centauri is a double star consisting of a yellow supergiant primary (V810 Cen A) and blue giant secondary (V810 Cen B). It is a small amplitude variable star, entirely due to the supergiant primary which is visually over three magnitudes brighter than the secondary. It is the MK spectral standard for class G0 0-Ia. V810 Cen A shows semi-regular variations with several component periods. The dominant mode is around 156 days and corresponds to Cepheid fundamental mode radial pulsation.
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Xi Ursae Majoris (ξ Ursae Majoris, abbreviated Xi UMa, ξ UMa), also named Alula Australis , is a star system in the constellation of Ursa Major. On May 2, 1780, Sir William Herschel discovered that this was a binary star system, making it the first such system ever discovered. It was the first visual double star for which an orbit was calculated, when it was computed by Félix Savary in 1828. It is also a variable star with a small amplitude.
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Friedrich Georg Wilhelm von Struve Struve's name is best known for his observations of double stars, which he carried on for many years. Although double stars had been studied earlier by William Herschel and John Herschel and Sir James South, Struve outdid any previous efforts. He discovered a very large number of double stars and in 1827 published his double star catalogue Catalogus novus stellarum duplicium. Stars of his catalogue are sometimes indicated by the Greek letter sigma, Σ. Thus, 61 Cygni is also designated as Σ2758.
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It included the bright stars of Crux, the southern part of Centaurus, Circinus, at least one star in Lupus, the bright stars of Musca, Beta and the optical double star Delta1,2 Chamaeleontis: and some of the stars of Volans, and Mensa. The Kalapalo people of Mato Grosso state in Brazil saw the stars of Crux as Aganagi angry bees having emerged from the Coalsack, which they saw as the beehive. Among Tuaregs, the four most visible stars of Crux are considered iggaren, i.e. four Maerua crassifolia trees.
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HD 119921 is a single, white-hued star in the southern constellation of Centaurus. it has the Bayer designation z Centauri. This is faintly visible to the naked eye, having an apparent visual magnitude of 5.15. It forms a wide double star with a faint, magnitude 12.50 visual companion, which is located at an angular separation of as of 2010. HD 119921 is moving closer to us with a heliocentric radial velocity of around −10 km/s, and is currently located some from the Sun.
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Nu Aquilae (ν Aql, ν Aquilae) is the Bayer designation for a double star in the constellation of Aquila and lies close to the celestial equator. It has an apparent visual magnitude of 4.72 and so is visible to the naked eye. The spectrum of ν Aql A matches a stellar classification of F3, with the luminosity class of Ib indicating this is a supergiant. The outer atmosphere has an effective temperature of 6,700 K and it has the yellow-white hue of an F-type star.
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Lambda Arietis (λ Ari, λ Arietis) is the Bayer designation for a double star in the northern constellation of Aries. Based upon an annual parallax shift of 25.32 arcseconds, this system is approximately distant from Earth. The pair have a combined apparent visual magnitude of 4.79, which is bright enough to be viewed with the naked eye. Because the yellow secondary is nearly three magnitudes fainter than the white primary, they are a challenge to split with quality 7× binoculars and are readily resolvable at 10×.
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In Heinlein's 1956 novel Double Star, humans have colonized the solar system, and a politician on Mars faces the civil rights issue of granting a native Martian species (who are second- class citizens) the right to vote. In Philip K. Dick's novel Martian Time-Slip (1964), a human colony on Mars is trying to cope with arduous environmental conditions. They treat an aboriginal race, whom they call "Bleekmen", with casual racism. In The Three Stigmata of Palmer Eldritch (1965), Mars has no indigenous life.
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Kappa Herculis (κ Herculis, abbreviated Kappa Her, κ Her) is an optical double star in the constellation of Hercules. The two components, Kappa Herculis A (Marsic , the traditional name of the system) and B, were 27.3 arc seconds apart in 2000. Based on parallax measurements from the Hipparcos mission, κ Her A is about 113 parsecs (370 light-years) from the Sun and κ Her B is 600 parsecs (2,000 light-years). A faint third component Kappa Herculis C is just over 1 arc-minute away.
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Beta, Delta and Zeta constitute the Tien Kang ("heavenly rope") in China.Richard Hinckley Allen: Star Names — Their Lore and Meaning: Piscis Australis, the Southern Fish Beta is a white main sequence star of apparent magnitude 4.29 that is of similar size and luminosity to Fomalhaut but five times as remote, at around 143 ± 1 light- years distant from Earth. Delta Piscis Austrini is a double star with components of magnitude 4.2 and 9.2. The brighter is a yellow giant of spectral type G8 III.
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The Wellington City Council purchased the telescope for £2000 in 1923, and the telescope was shipped from Napier to Wellington. It was later transferred to the care of the Carter Observatory under the Carter Observatory Act (1938). At the Carter Observatory site, the Cooke telescope was used for solar astronomy research as well as flare star and double star monitoring programs over the following decades. In April 1968, Carter Observatory was one of the observatories involved in recording an occultation of Neptune by the Moon.
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Alpha Librae (α Librae, abbreviated Alpha Lib, α Lib) is a double star and, despite its 'alpha' designation, it is the second-brightest star system (or star) in the constellation of Libra. The two components are designated α¹ Librae and α² Librae. The system bore the traditional name of Zubenelgenubi , though the International Astronomical Union now regards that name as only applying to α² Librae. Alpha² Librae is 0.33 degrees north of the ecliptic so it can be occulted by the Moon and (very rarely) by planets.
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The Albireo system is a double star designated Beta Cygni (β Cygni, abbreviated Beta Cyg, β Cyg). The International Astronomical Union uses the name "Albireo" specifically for the brightest star in the system. Although designated 'beta', it is fainter than Gamma Cygni, Delta Cygni, and Epsilon Cygni and is the fifth-brightest point of light in the constellation of Cygnus. Appearing to the naked eye to be a single star of magnitude 3, viewing through even a low-magnification telescope resolves it into its two components.
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It is designated as component C in the Catalog of Components of Double and Multiple Stars, not to be confused with component C in the Washington Double Star Catalog which is a faint optical companion. An orbit for the pair has since been computed using interferometric measurements, but as only approximately a quarter of the orbit has been observed, the orbital parameters must be regarded as preliminary. The period of this orbit is 214 years. The status of the two possible companions is still not clarified.
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90 Tauri (90 Tau) is a star in the zodiac constellation of Taurus, located 144 light years away from the Sun. It is visible to the naked eye as a faint, white-hued star with an apparent visual magnitude of 4.27. 90 Tauri is a member of the Hyades cluster and is listed as a double star. This is an A-type main-sequence star with a stellar classification of A6 V. It has 2.1 times the mass of the Sun and 2.8 times the Sun's radius.
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36 Ursae Majoris is a double star in the northern constellation of Ursa Major. With an apparent visual magnitude of 4.82, it can be seen with the naked eye in suitable dark skies. Based upon parallax measurements, this star lies at a distance of from Earth. This star is a solar analog—meaning it has physical properties that make it similar to the Sun. It has 12% more mass and a radius 15% larger than the Sun, with an estimated age of 2.7 billion years.
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Kappa1 Lupi is a solitary star in the southern constellation of Lupus. It is visible to the naked eye with an apparent visual magnitude of 3.86, and forms a double star with Kappa2 Lupi. Based upon an annual parallax shift of 18.12 mas as seen from Earth, it is located about 180 light years from the Sun. Both Kappa1 Lupi and its neighbor Kappa2 Lupi are members of the Hyades Stream, which is a moving group that is coincident with the proper motions of the Hyades cluster.
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57 Cancri is a double star in the zodiac constellation of Cancer, located around 460 light years away from the Sun. They are visible to the naked eye as a faint star with a combined apparent visual magnitude of +5.40. The brighter member, designated component A. is a yellow-hued giant star with a stellar classification of G7 III and an apparent magnitude of +6.09. Its companion, component B, is an orange-hued giant with a class of K0 III and an apparent magnitude of +6.37.
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These stars are short period (six hours at most) pulsating stars that have been used as standard candles and as subjects to study astroseismology. Delta Boötis is a wide double star with a primary of magnitude 3.5 and a secondary of magnitude 7.8. The primary is a yellow giant that has cooled and expanded to 10.4 times the diameter of the Sun. Of spectral class G8IV, it is around 121 light-years away, while the secondary is a yellow main sequence star of spectral type G0V.
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11 Camelopardalis and its reddish companion 12 Camelopardalis 11 Camelopardalis is a single star in the northern circumpolar constellation of Camelopardalis, located around 710 light years away from the Sun as determined by parallax. It has the variable star designation BV Camelopardalis; 11 Camelopardalis is the Flamsteed designation. This object is visible to the naked eye as a faint, blue-white hued star with a baseline apparent visual magnitude of +5.22. It forms a double star with 12 Camelopardalis, which is only 3 arcminutes away.
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The Washington Double Star Catalog gives a magnitude of 10.48 and the Catalog of Components of Double and Multiple Stars a magnitude of 11.5. Component D has an early B spectral type, near B3. The full MK spectral type has been measured as B2 IV, and the assumption of a subgiant luminosity suggests that it is more distant than the other stars of the system. The spectral type has also been estimated photometrically as B2 V, and a main sequence luminosity matches the distance of the other stars.
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1051-1061, , . Another star, CCDM J21483-4718B (also designated CD−47 13929 or WDS J21483-4718B), of apparent visual magnitude 8.7, has been observed 55 arcseconds away from this star,CCDM J21483-4718, database entry, CCDM (Catalog of Components of Double & Multiple stars), J. Dommanget and O. Nys, second edition, 2002, VizieR database I/274. but based on comparison of proper motions, it is believed to be an optical double and not physically related to its companion.Notes, WDS 21483-4718, The Washington Double Star Catalog, B. D. Mason et al.
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Assuming that one of the fifteen stars on the map must represent Earth's Sun, Fish constructed a three-dimensional model of nearby Sun-like stars (i.e. stars deemed to have characteristics that could support life such as that found on Earth) using thread and beads, basing stellar distances on those published in the 1969 Gliese Star Catalogue. Studying thousands of vantage points over several years, the only one that seemed to match the Hill map was from the viewpoint of the double star system of Zeta Reticuli. Fish sent her analysis to Webb.
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The full eclipse of the small blue star by the orange giant lasts 38 days, with two partial phases of 32 days at the beginning and end. The primary has a diameter of 150 D☉ and a luminosity of ; the secondary has a diameter of 4 D☉ and a luminosity of . Zeta Aurigae was spectroscopically determined to be a double star by Antonia Maury in 1897 and was confirmed as a binary star in 1908 by William Wallace Campbell. The two stars orbit each other about apart.
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Unusually, a total of 15 of the 23 brightest stars in Crux are spectrally blue-white B-type stars. Among the five main bright stars, Delta, and probably Alpha and Beta, are likely co- moving B-type members of the Scorpius–Centaurus Association, the nearest OB association to the Sun. They are among the highest-mass stellar members of the Lower Centaurus-Crux subgroup of the association, with ages of roughly 10 to 20 million years. Other members include the blue-white stars Zeta, Lambda and both the components of the visual double star, Mu.
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HD 2767 is the primary component of a double star located away in the constellation Andromeda. It is a red giant with a spectral type of K1III and an apparent magnitude of 5.88, thus is visible by the naked eye under favourable conditions. The secondary is named BD+32 81, has an apparent magnitude of 9.28, and is an F-type star; it shares radial velocity, parallax and proper motion with the primary component. The distance from the primary is estimated as 6,536 AU, while their separation in the sky is 56 arcseconds.
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Double Star is a two-player game about space warfare, and operates on the belief that warfare between two star systems is possible but expensive and difficult. This game is based in a binary star system, where the two stars orbit each other, and each star has a different colony orbiting it. Each colony has both antipathy for the other colony and something the other colony needs, and so war begins. The board features both worlds as they orbit their respective stars, and both stars orbiting each other.
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May be played in an afternoon." In the March 1980 edition of Dragon (Issue 35), William Fawcett enjoyed the ability to choose tactical formations for space fleets, and liked the rules, which he found to be simple enough to digest in 30 minutes. "There appear to be no serious ambiguities or omissions, although your first few spaceship-to-spaceship combats may drag a little until you become familiar with the formation system." Fawcett recommended the game, saying, "Double Star is one of the most solid science-fiction games this reviewer has played.
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NOEMA has observed the most distant galaxy known to date. Together with the IRAM 30-meter telescope it made the first complete and detailed radio images of nearby galaxies and their gas. NOEMA also obtained the first image of a gas disk surrounding a double star system (Guilloteau et al. 1994). Its antennas captured for the first time a cavity in one of these disks, a major hint for the existence of a planetary object orbiting the new star and absorbing matter on its trajectory (GG tau, Piétu et al. 2011).
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Chi Ceti (χ Ceti), is the Bayer designation for a double star in the equatorial constellation of Cetus. They appear to be common proper motion companions, sharing a similar motion through space. The brighter component, HD 11171, is visible to the naked eye with an apparent visual magnitude of 4.66, while the fainter companion, HD 11131, is magnitude 6.75. Both lie at roughly the same distance, with the brighter component lying at an estimated distance of 75.6 light years from the Sun based upon an annual parallax shift of 43.13 mass.
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Galileo observed the Milky Way, previously believed to be nebulous, and found it to be a multitude of stars packed so densely that they appeared from Earth to be clouds. He located many other stars too distant to be visible with the naked eye. He observed the double star Mizar in Ursa Major in 1617. In the Starry Messenger, Galileo reported that stars appeared as mere blazes of light, essentially unaltered in appearance by the telescope, and contrasted them to planets, which the telescope revealed to be discs.
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It is a double star with a magnitude 9.3 companion at an angular separation of 0.6 arcseconds along a position angle of 257°. The stellar classification of this star is F0 V; hence it belongs to the category of F-type main sequence stars that generate energy through hydrogen fusion at the core. It is 1.8 billion years old with 1.35 times the mass of the Sun and 1.79 times the Sun's radius. The star is radiating 6.1 times the luminosity of the Sun from its photosphere at an effective temperature of 6,806 K.
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The WGSN approved the name Piautos for Lambda Cancri on 1 June 2018 and it is now so included in the List of IAU-approved Star Names. The WGSN had previously stated that where a component letter (from e.g. Washington Double Star Catalog) is not explicitly listed, that the name should be understood to be attributed to the brightest component by visual brightness (Lambda Cancri A in this case). In Chinese, (), meaning Beacon Fire, refers to an asterism consisting of Lambda Cancri and Psi, Phi1 and 15 Cancri.
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In October 1842, Wilhelm Struve found that γ2 Andromedae was itself a double star whose components were separated by less than an arcsecond. The components are an object of apparent visual magnitude 5.5, γ Andromedae B, and a type-A main sequence star with apparent visual magnitude 6.3, γ Andromedae C. They have an orbital period of about 64 years. Spectrograms taken from 1957 to 1959 revealed that γ Andromedae B was itself a spectroscopic binary, composed of two type-B main sequence stars orbiting each other with a period of 2.67 days.
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23 Orionis is a double star located around 1,200 light years away from the Sun in the equatorial constellation of Orion. It is visible to the naked eye as a dim, blue-white hued point of light with a combined apparent visual magnitude of 4.99. The pair are moving away from the Earth with a heliocentric radial velocity of +18 km/s, and they are members of the Orion OB1 Association, subgroup 1a. Howe and Clarke (2009) catalog this as a double-lined spectroscopic binary star system with a wide projected separation of .
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He was born on 10 November 1861 in Edinburgh to John and Elizabeth (née Ayton) Innes. He had 11 younger siblings. A self-taught astronomer, he went to Australia at an early age and made his living as a wine merchant in Sydney, where, using a home made 12-inch reflecting telescope, he discovered several double stars new to astronomy. The picture shown is probably Van den Bos Innes published a double star catalog in 1900 that assimilated all earlier observations by southern astronomers, to provide the longest baseline for orbit determination.
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It is later revealed that Tia is not unusual in this respect, but Tony is; few of their kind have the ability to speak out loud. After their foster guardian, Mrs. Malone, dies, they are placed by social services in a juvenile detention home under grim, unwholesome conditions, where Tia befriends a black cat, Winkie. Both have suppressed memories of their past, but discover a clue in an old road map hidden along with a cache of money in Tia's "star box", a leather purse-like box with a double-star design on it.
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First run in 1938, the A.82 was a more powerful development of the A.80, itself derived from the A.74, which powered the Breda Ba.65 and Fiat BR.20. It was claimed to be 50% more powerful than its antecedents and one of the most powerful engines produced by the country. It was the largest Italian engine design of the time. The A.82 was an 18 cylinder radial, consisting of two rows of nine cylinders arranged in a double star with a triple throw crankcase made of aluminium alloy.
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Both stars in the KZ Andromedae system are main sequence stars of spectral type K2Ve, meaning that the spectrum shows strong emission lines. This is caused by their active chromosphere that cause large spots on the surface. KZ Andromedae is listed in the Washington Double Star Catalog as the secondary component in a visual binary system, with the primary being HD 218739. In 50 years of observations, there is little evidence of relative motion between the two stars; however, they have a common proper motion and a similar radial velocity.
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The Burnham Double Star Catalogue (BDS) is a catalogue of double stars within 121° of the celestial North Pole. It was published in two parts by the Carnegie Institution of Washington in 1906, under the title A General Catalogue of Double Stars Within 121° of the North Pole. The first part gives coordinates, designations, and magnitudes for 13,665 pairs of double stars, comprising almost all double stars discovered before 1906.A General Catalogue of Double Stars Within 121° of the North Pole, Part I, Sherburne Wesley Burnham, Carnegie Institution of Washington, 1906.pp.
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This is believed to be a solitary star, although it has a faint optical companion at an angular separation of 13.5 arcseconds, making it a double star. The stellar classification of Alpha Columbae is B7 IV, with the luminosity class of IV indicating it has evolved into a subgiant star. The spectrum shows it to be a Be star surrounded by a hot gaseous disk, which is generating emission lines because of hydrogen recombination. Like most if not all such stars, it is rotating rapidly with a projected rotational velocity of .
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This was found to be a double star by R. A. Rossiter in 1953, with the magnitude 13.7 companion having an angular separation of along a position angle of 266°, as of 2016. The brighter, magnitude 4.32 component A is a spectroscopic binary. As of 2009, the orbital solution for this pair is of low quality, giving a period of roughly and an eccentricity of around 0.4. The primary component is an aging giant star with a stellar classification of , where the suffix notation indicates an underabundance of the cyanogen molecule.
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In September 2013, Haddadi signed with the Sichuan Blue Whales of the Chinese Basketball Association as the bonus foreign Asian player that's allowed to be on the expansion CBA team. On September 15, 2014, Haddadi agreed to terms with Qingdao DoubleStar Eagles.Qingdao Double Star agreed to terms with Hamed Haddadi With Haddadi's help, the Eagles were one of the top teams during the 2014–15 season. During his time in Qingdao, Haddadi would average 20.4 points, 13.9 rebounds, 3.7 assists, and 2.3 blocks for the team's surprise rise.
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Struve 2398 (Gliese 725) is a binary star system in the northern constellation of Draco. Struve 2398 is star number 2398 in the Struve Double Star Catalog of Baltic-German astronomer Friedrich Georg Wilhelm von Struve. The astronomer's surname, and hence the star identifier, is sometimes indicated by a Greek sigma, Σ. Although the components are too faint to be viewed with the naked eye, this star system is among the closest to the Sun. Parallax measurements by the Hipparcos spacecraft give them an estimated distance of about 11.6 light years away.
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HD 222093 is a double star in the equatorial constellation of Aquarius. It has an orange hue and is visible to the naked eye with an apparent visual magnitude of 5.68. The system is located at a distance of approximately 293 light years from the Sun based on parallax, but is drifting closer with a radial velocity of −13 km/s. The primary component is an aging K-type giant star with a stellar classification of K0III, which indicates it has exhausted the supply of hydrogen at its core then cooled and expanded.
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Mu Cassiopeiae (μ Cassiopeiae, abbreviated μ Cas) is a binary star system in the constellation Cassiopeia. This system shares the name Marfak with Theta Cassiopeiae, and the name was from Al Marfik or Al Mirfaq (المرفق), meaning "the elbow". Mu Cassiopeiae is given as a standard star for the spectral class G5Vb, although it is frequently described as a subdwarf, meaning it has a luminosity below that expected for a G5 main sequence star. There are five visible companions to Mu Cassiopeiae listed in the Washington Double Star Catalog.
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Gamma Herculis is also a double star divisible in small amateur telescopes. The primary is a white giant of magnitude 3.8, 195 light- years from Earth. The optical companion, widely separated, is 10th magnitude. Zeta Herculis is a binary star that is becoming divisible in medium-aperture amateur telescopes, as the components widen to their peak in 2025. The system, 35 light-years from Earth, has a period of 34.5 years. The primary is a yellow-tinged star of magnitude 2.9 and the secondary is an orange star of magnitude 5.7.
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It is approximately 63 times as luminous the Sun, with a surface temperature of 5279 K. Delta Apodis is a double star, the two components of which are 103 arcseconds apart and visible through binoculars. Delta1 is a red giant star of spectral type M4III located 630 ± 30 light-years away. It is a semiregular variable that varies from magnitude +4.66 to +4.87, with pulsations of multiple periods of 68.0, 94.9 and 101.7 days. Delta2 is an orange giant star of spectral type K3III, located 550 ± 10 light-years away, with a magnitude of 5.3.
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Xi Pegasi (ξ Peg, ξ Pegasi) is the Bayer designation for a double star in the northern constellation of Pegasus, the winged horse. Located in the horse's neck, the primary component is an F-type main sequence star that is visible to the naked eye with an apparent visual magnitude of 4.2. It is 86% larger and 17% more massive that the Sun, radiating 4.5 times the solar luminosity. Based upon parallax measurements taken with the Hipparcos spacecraft, it is located 53.2 ± 0.2 light years from the Sun.
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Mintaka is 915 light years away and shines with magnitude 2.21. It is 90,000 times more luminous than the Sun and is a double star: the two orbit each other every 5.73 days. In the Northern Hemisphere, Orion's Belt is best visible in the night sky during the month of January around 9:00 pm, when it is approximately around the local meridian. Just southwest of Alnitak lies Sigma Orionis, a multiple star system composed of five stars that have a combined apparent magnitude of 3.7 and lying 1150 light years distant.
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She was the first woman to be awarded the European Geosciences Union Julius Bartels Medal. Her research considers plasma flow and the configuration of the electromagnetic field in the magnetotail during substorms. She used data from the Geotail, Cluster II, THEMIS and Double Star missions to confirm that the earthward moving fast flows of the plasma sheet are bubbles of low density plasma that is accompanied by depolarization fronts. Nakamura investigated the shape and size of these fronts, and showed that field aligned currents flow into and out of the ionosphere at their meridional flanks.
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Mizar, in Ursa Major, was observed to be double by Benedetto Castelli and Galileo.A New View of Mizar, Leos Ondra, accessed on line May 26, 2007. The identification of other doubles soon followed: Robert Hooke discovered one of the first double-star systems, Gamma Arietis, in 1664, while the bright southern star Acrux, in the Southern Cross, was discovered to be double by Fontenay in 1685. Since that time, the search has been carried out thoroughly and the entire sky has been examined for double stars down to a limiting apparent magnitude of about 9.0.
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Astronomers have mistakenly reported observations of a double star in place of J 900 and a faint star in the constellation of Gemini. Observation of visual double stars by visual measurement will yield the separation, or angular distance, between the two component stars in the sky and the position angle. The position angle specifies the direction in which the stars are separated and is defined as the bearing from the brighter component to the fainter, where north is 0°.p. 2, Observing and Measuring Double Stars, Bob Argyle, ed.
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Mu Crucis, Latinized from μ Crucis, is the seventh-brightest star in the constellation Crux commonly known as the Southern Cross. μ Crucis is a wide double star of spectral class B stars, magnitude 4.0 and 5.2 respectively. They lie about 370 light-years away, and both stars are likely physically attached. The brighter component is known as μ1 Crucis or μ Crucis A, while the fainter is μ2 Crucis or μ Crucis B. μ1 Crucis is the brighter of the two stars with an apparent magnitude of 4.0.
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The white stars Beta and Gamma Trianguli, of apparent magnitudes 3.00 and 4.00, respectively, form the base of the triangle and the yellow-white Alpha Trianguli, of magnitude 3.41, the apex. Iota Trianguli is a notable double star system, and there are three star systems with known planets located in Triangulum. The constellation contains several galaxies, the brightest and nearest of which is the Triangulum Galaxy or Messier 33—a member of the Local Group. The first quasar ever observed, 3C 48, also lies within the boundaries of Triangulum.
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Portrait of Daniel Webster by J. A. Whipple, c. 1847 John Adams Whipple (September 10, 1822 – April 10, 1891) was an American inventor and early photographer. He was the first in the United States to manufacture the chemicals used for daguerreotypes; he pioneered astronomical and night photography; he was a prize-winner for his extraordinary early photographs of the moon; and he was the first to produce images of stars other than the sun (the star Vega and the Mizar-Alcor stellar sextuple system,)] which was thought to be a double star until 2009.
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This widely believed prediction has been occasionally tested using astronomical observations. For example, in a binary star system, the two stars are moving in opposite directions, and one might test the prediction by analyzing their light. (See, for instance, the De Sitter double star experiment.) Unfortunately, the extinction length of light in space nullifies the results of any such experiments using visible light, especially when taking account of the thick cloud of stationary gas surrounding such stars. However, experiments using X-rays emitted by binary pulsars, with much longer extinction length, have been successful.
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The WGSN approved the name Syrma for Iota Virginis on 12 September 2016 and it is now so included in the List of IAU-approved Star Names. For such names relating to members of multiple star systems, and where a component letter (from e.g. Washington Double Star Catalog) is not explicitly listed, the WGSN says that the name should be understood to be attributed to the brightest component by visual brightness. In China, (), meaning Neck, refers to an asterism consisting of this star, Kappa Virginis, Phi Virginis and Lambda Virginis.
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Theta Tauri (θ Tauri, abbreviated Theta Tau, θ Tau) is a wide double star in the constellation of Taurus and a member of the Hyades open cluster. θ Tauri is composed of two 3rd magnitude stars, designated Theta¹ Tauri (Theta Tauri B) and Theta² Tauri (Theta Tauri A). Theta² is brighter, hence the pair are sometimes referred to as Theta Tauri B and A, respectively. They are separated by 5.62 arcminutes (0.094°) on the sky. Based upon parallax measurements, Theta¹ Tauri is located at a distance of , while Theta² Tauri is at a distance of .
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Pleiades and Hyades with κ Tauri as the very close pair at lower centre (north is approximately to the left) The system is dominated by a visual double star, κ1 Tauri and κ2 Tauri. κ1 Tauri is a white A-type subgiant with an apparent magnitude of +4.22. It is emitting an excess of infrared radiation at a temperature indicating there is a circumstellar disk in orbit at a radius of 67 AU from the star. κ2 Tauri is a white A-type main sequence star with an apparent magnitude of +5.24.
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21 Tauri, formally known as Asterope , is a component of the Asterope double star in the Pleiades open cluster. 21 Tauri is the stars' Flamsteed designation. This star is potentially faintly visible to the naked eye with an apparent visual magnitude of 5.76 in ideal conditions, although anybody viewing the object is likely to instead see the pair as a single elongated form of magnitude 5.6. The distance to 21 Tauri can be estimated from its annual parallax shift of , yielding a range of around 431 light years.
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Pi Tucanae (π Tuc, π Tucanae) is a double star in the southern constellation of Tucana. It is visible to the naked eye with a combined apparent visual magnitude of +5.49. Based upon an annual parallax shift of 10.25 mas as seen from Earth, it is located around 317 light years from the Sun. The brighter star, component A, is a B-type main sequence star with a stellar classification of B9 V. At an age of about 206 million years, it is spinning rapidly with a projected rotational velocity of 236.
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Arundhati (, IAST: Arundhatī) is the wife of the sage Vashistha, one of the seven sages (Saptarshi) who are identified with the Ursa Major. She is identified with the morning star and also with the star Alcor which forms a double star with Mizar (identified as Vashista Maharshi) in Ursa Major. Arundhati, though the wife of one of the seven seers, is accorded the same status as the seven seers and is worshipped with them as such. In the Vedic and Puranic literature, she is regarded as the epitome of chastity, conjugal bliss and wifely devotion.
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HD 1185 is a double star in the northern constellation of Andromeda. The primary, with an apparent magnitude of 6.15, is a white main-sequence star of spectral type A1Si, indicating it has stronger silicon absorption lines than usual, thus making it also an Ap star. The secondary companion, which is 9.08 arcseconds away, is not visible to the naked eye at an apparent magnitude of 9.76, and is also an A-type star. It shares common proper motion and parallax with the primary star but orbital parameters are still unknown.
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Fortria returned to Cheltenham to contest the Champion Chase, which had been run for the first time in 1959. As the previous winner, Quita Que, was injured, Fortria was sent off the 2/1 favourite against Double Star and Blue Dolphin. Fortria contested the lead with Flame Gun (winner of the 1959 Cotswold Chase), who fell at the third last, before winning by three lengths from Blue Dolphin. Fortria completed his season by running in the Galway Plate under 12 st 7 lbs, where he finished fourth to Sparkling Flame.
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In September 2014, he returned to China and signed with the Qingdao Eagles for the 2014–15 CBA season.Qingdao Double Star on fire, finalizing deal with Mike Harris On April 10, 2015, he re-signed with Leones de Ponce.Mike Harris signs with Leones de Ponce In October 2015, he signed with Sichuan Blue Whales for the 2015–16 CBA season. Harris helped lead Sichuan to their first-ever CBA title the following March, and re-signed with the Blue Whales for the 2016-17 CBA season, but missed much of the campaign with an injury.
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Rho1 Cephei (ρ1 Cephei) is a double star located in the northern constellation of Cepheus. As of 2014, the pair had an angular separation of 0.29 arc seconds along a position angle of 211.1°. This corresponds to a projected separation of 18.1 AU. Rho1 Cephei is faintly visible to the naked eye with an apparent visual magnitude of 5.84, and it forms an optical pair with the brighter star Rho2 Cephei. Based upon an annual parallax shift of 15.83 mas as seen from the Earth, Rho1 Cephei is located about 206 light years from the Sun.
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This minor planet was named after Sherburne Wesley Burnham (1838–1921), American astronomer who discovered many visual binary stars and is known for his Burnham Double Star Catalogue (BDS), a catalogue of double stars seen in the Northern Hemisphere, which was published in two parts by the Carnegie Institution of Washington in 1906. Burnham observed from the Chicago (1877), Lick (1888) and Yerkes (1897) observatories. The was published in the journal Astronomische Nachrichten in 1921 (), and was also mentioned in The Names of the Minor Planets by Paul Herget in 1955 (). The lunar crater Burnham is also named in his honor.
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Delta Persei (Delta Per, δ Persei, δ Per) is a double star in the northern constellation of Perseus. It has an apparent visual magnitude of 3.01, making it readily visible with the naked eye. Parallax measurements give it a distance of about from the Earth. The spectrum of this star matches a stellar classification of B5 III, which indicates it is a giant star that has evolved away from the main sequence after exhausting the hydrogen at its core. It has about seven times the Sun's mass and has an estimated age of 6.8 million years.
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Blanche Descartes, Network-colourings, The Mathematical Gazette (London) 32, 67-69, 1948.Martin Gardner, The Last Recreations: Hydras, Eggs, and Other Mathematical Mystifications, Springer, 2007, , In 1973, George Szekeres found the fifth known snark — the Szekeres snark. In 1975, Rufus Isaacs generalized Blanuša's method to construct two infinite families of snarks: the flower snark and the BDS or Blanuša–Descartes–Szekeres snark, a family that includes the two Blanuša snarks, the Descartes snark and the Szekeres snark. Isaacs also discovered a 30-vertices snark that does not belong to the BDS family and that is not a flower snark: the double-star snark.
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Jonas Björkman successfully defended his Australian Open doubles title. Patrick Rafter became one of the few men to hold a singles and doubles Grand Slam title simultaneously. Last year's double star and defending champion Jacco Eltingh retired at the end of the previous year, so his former partner Jonas Björkman teamed up with countryman Patrick Rafter as the fifth seed. The other top seeds were "Indian Express" (Mahesh Bhupathi and Leander Paes) at No. 1, the "Woodies" (Todd Woodbridge and Mark Woodforde) at No. 2, Mark Knowles and Daniel Nestor at No. 3, and Ellis Ferreira and Rick Leach at No. 4.
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Oleg Sirotin (2014). Double Star: Aleksandr and Ivan Mozzhukhin double biography in the Penza Regional Library, electronic version (in Russian)Oleg Sirotin. Family and fatherland of Ivan Mozzhukhin article from the Notes on Film Studies magazine, main editor Naum Kleiman (2006, in Russian) While all three elder brothers finished seminary, Ivan was sent to the Penza gymnasium for boys and later studied law at the Moscow State University. In 1910, he left academic life to join a troupe of traveling actors from Kiev, with which he toured for a year, gaining experience and a reputation for dynamic stage presence.
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AG Persei is another Algol variable in Perseus, whose primary component is a B-type main sequence star with an apparent magnitude of 6.69. Phi Persei is a double star, although the two components do not eclipse each other. The primary star is a Be star of spectral type B0.5, possibly a giant star, and the secondary companion is likely a stellar remnant. The secondary has a similar spectral type to O-type subdwarfs. With the historical name Mirfak (Arabic for elbow) or Algenib, Alpha Persei is the brightest star of this constellation with an apparent magnitude of 1.79.
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Miller, Chadwick, Harshman, and Wiseman designed Traveller, which was published in 1977 by GDW. Miller designed the science-fiction board game Double Star for GDW which was released in 1979. While at GDW, Miller designed a total of 74 games and products, with an average of one every four months, including Imperium; and, co-designed MegaTraveller and 2300 AD. Miller wrote a letter to the company, Digest Group Publications (DGP), in 1987 asking them to help GDW make Traveller material more accessible. Despite being some of the best Traveller material published, DGP produced considerable work that went unused.
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In July 2015, Lucas signed with the Chinese team Qingdao DoubleStar,Kalin Lucas signs with Qingdao Double Star but was let go after a tryout period. He subsequently re-signed with TED Ankara Kolejliler in August 2015.TED Kolejliler Ankara extends the deal with Kalin Lucas Lucas was selected to compete in the Turkish League's All-Star Skills Challenge but had to withdraw due to injury.Recap of Spor Toto All-Star 2016 On October 29, 2016, Lucas was reacquired by the Iowa Energy. In 14 games, he averaged 16.9 points, 5.1 assists, 3.9 rebounds, and 1.1 steals.
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It has a surface temperature of 5180 K. For most of its existence, Delta Coronae Borealis was a blue-white main-sequence star of spectral type B before it ran out of hydrogen fuel in its core. Its luminosity and spectrum suggest it has just crossed the Hertzsprung gap, having finished burning core hydrogen and just begun burning hydrogen in a shell that surrounds the core. Zeta Coronae Borealis is a double star with two blue-white components 6.3 arcseconds apart that can be readily separated at 100x magnification. The primary is of magnitude 5.1 and the secondary is of magnitude 6.0.
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Both stars are members of Scorpius-Centaurus Association or the smaller portion known as the Lower Centaurus Crux subgroup. The double star forms the nucleus of the very young Epsilon Chamaeleontis stellar group which comprises about twenty stars. The nebulosity and star formation occurring in this region is currently a very important line of study in the southern hemisphere, whose proximity to the Sun is yielding new astrophysical information. Several papers have been published in the last few years on Lower Centaurus Crux subgroup of stars in the far southern constellations of Musca, Chamaeleon and Octans holding the south celestial pole.
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After completing her undergraduate work, Maury went to work at the Harvard College Observatory as one of the so-called Harvard Computers, highly skilled women who processed astronomical data. Her salary was 25 cents, half the amount paid to men at that time. In 1887, Edward Charles Pickering had found the first spectroscopic binary or double star, ζ1 Ursae Majoris (Mizar A). Maury was asked to determine its orbit, which she did using periodic doubling of some of the lines in its spectrum. Then, in 1889, Maury discovered a second spectroscopic binary, Beta Aurigae, and calculated its orbital period.
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Eric E. Mamajek proposed the name Luhman 16 for the system, with the components called Luhman 16A and Luhman 16B. The name originates from the frequently updated Washington Double Star Catalog (WDS): Luhman has already published several new discoveries of binary stars that have been compiled in the WDS with discovery identifier "LUH". The WDS catalog now lists this system with the identifier 10493−5319 and discoverer designation LUH 16. The rationale is that Luhman 16 is easier to remember than WISE J104915.57−531906.1 and that "it seems silly to call this object by a 24-character name (space included)".
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Psi Cassiopeiae (ψ Cassiopeiae) is a binary star system in the northern constellation of Cassiopeia. The primary component, ψ Cassiopeiae A, is an orange K-type giant with an apparent magnitude of +5.0; it is a double star, designated CCDM J01259+6808AB, with a fourteenth magnitude star (component B) located 3 arcseconds from the primary. Located about 25 arcseconds distant there is a 9.8 magnitude optical companion CCDM J01259+6808CD, designated ψ Cassiopeiae B in older star catalogues, which is itself another double; CD comprises a 9.4 magnitude component C and a 10 magnitude component D.
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Gamma Andromedae (γ Andromedae, abbreviated Gamma And, γ And) is the third- brightest point of light in the constellation of Andromeda. It is a multiple star system approximately 350 light-years from the Earth. In 1778, Johann Tobias Mayer discovered that γ Andromedae was a double star. When examined in a small telescope, it appears to be a bright, golden-yellow star (γ1 Andromedae or γ Andromedae A, officially named Almach , the traditional name for the entire system) next to a dimmer, indigo-blue star (γ2 Andromedae or γ Andromedae B), separated by approximately 10 arcseconds.
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During the Age of Enlightenment, several hundred Jewish families were granted arms throughout Europe and were made part of the Nobility. Such as the Rothchilds, Montefiores, Goldsmids and Sassoon families, who were all granted arms and noble titles in England. Many wealthy British Jews would once again adopt the heraldic customs of their country while still retaining many Jewish elements. However, during the first and second Aliyah, many British Jews adopted Zionist symbolisms on the arms such as Sir Moses Montefiore, who adopted a Zionist tree and flag on his arms, alongside a double star of David.
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Kaj Strand was born February 27, 1907 in Hellerup, Denmark, on the outskirts of Copenhagen. He entered the University of Copenhagen in 1926, majored in astronomy, and graduated in 1931 with Magister (Master's) and Candidate Magister degrees. At the invitation of Ejnar Hertzsprung, during the 1930s he worked at Leiden on a program of photographing double stars; he applied these results toward his doctorate from Copenhagen in 1938. From 1938-42 Strand worked under Peter van de Kamp as a Research Associate at Swarthmore College, and began the photographic double star program with the refractor telescope at the college's Sproul Observatory.
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1 Geminorum (1 Gem) is a star in the constellation Gemini. Its apparent magnitude is 4.15. In the 19th century, John Flamsteed numbered the brighter stars, by constellation, from west to east, and 1 Geminorum was the first star listed in Gemini. It is also listed in the Bright Star Catalogue as star 2134, usually designated HR 2134 with the HR standing for the Harvard Revised catalog, the precursor to the Bright Star Catalogue. In 1948, 1 Geminorum was discovered to be a close double star whilst using it to focus a telescope for observations of the planet Uranus.
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Both stars in the FF Andromedae system are main sequence red dwarfs of spectral type M1Ve, meaning that the spectrum shows strong emission lines. The lines identified are H-alpha and CaII. They have a total mass of 1.10 and both are tidally locked, thus their rotation period is equal to the orbital period of 2.17 days. The secondary component should not be confused with the 13th magnitude star listed in the Washington Double Star Catalog as WDS J00428+3533B and sometimes referred to as GJ 29.1B, which is just a line-of-sight giant star much more distant than FF Andromedae.
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R Carinae is a double star in the southern constellation of Carina. The brighter component is a variable star that can be viewed with the naked eye at peak brightness, but is usually too faint to be seen without a telescope, having an apparent visual magnitude that fluctuates around 7.43. This star is located at a distance of approximately 1,300 light years from the Sun based on parallax, and is drifting further away with a radial velocity of +28 km/s. The main component is an aging red giant star on the asymptotic giant branch with a stellar classification of M6/7pe.
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This is an evolved giant star of type G with a stellar classification of G7 III. At the age of 360 million years, it has an estimated 3.1 times the mass of the Sun and has expanded to around 16 times the Sun's radius. The star is radiating 160 times the Sun's luminosity from its expanded photosphere at an effective temperature of 4,923 K. This star has an optical visual companion, CCDM J20500-3347B, of apparent visual magnitude 10.0 approximately 20.4 arcseconds away at a position angle of 166°.Entry 20500-3347, The Washington Double Star Catalog , United States Naval Observatory.
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Denebola , designated Beta Leonis (β Leonis, abbreviated Beta Leo, β Leo) is the second-brightest star in the zodiac constellation of Leo, although the two components of the γ Leonis double star, which are unresolved to the naked eye, have a combined magnitude brighter than it. Denebola is an A-type main sequence star with 75% more mass than the Sun and 15 times the Sun's luminosity. Based on parallax measurements from the Hipparcos astrometry satellite, the star is at a distance of about from the Sun. Its apparent visual magnitude is 2.14, making it readily visible to the naked eye.
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The minimum in i(G) is taken over less elements (only the independent sets are considered), so γ(G) ≤ i(G) for all graphs G. The inequality can be strict - there are graphs G for which γ(G) < i(G). For example, let G be the double star graph consisting of vertices x1, ..., xp, a, b, y1, ..., yq, where p, q > 1. The edges of G are defined as follows: each xi is adjacent to a, a is adjacent to b, and b is adjacent to each bj. Then γ(G) = 2 since {a, b} is a smallest dominating set.
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For 7 March 2017, a stellar occultation by Orcus had been predicted to take place in the Americas and over the Pacific Ocean. Observations were made at five sites in North and South America, and two solid body chords have been observed. Using speckle imaging, the occulted star was revealed to be a close double star, and a reconstruction of the orbits of Orcus and Vanth showed that both chords were from Vanth (occulting either of the two stars) rather than Orcus. A non-detection at a nearby site placed a constraint of () on the diameter of Vanth.
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A diagram of HD 53706 and HD 53680, relative to HD 53705 (Click to enlarge). HD 53705 was discovered to be a visual binary very early on, owing to the brightness of the two components. The earliest observation in the Washington Double Star Catalog (WDS) dates to 1826 and was made by James Dunlop, stating a position angle of 119 degrees and a separation of 21.5 arcseconds for the companion. The two stars have moved very little relative to each other since, with the most recent measurement from 1999 stating a position angle of 126 degrees and a separation of 20.9 arcseconds.
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A primary star, which is brighter and typically bigger than its companion stars, is designated by a capitalized A. Its companions are labelled B, C, and so on. For example, Sirius, the brightest star in the sky, is actually a double star, consisting of the naked- eye visible Sirius A and its dim white-dwarf companion Sirius B. The first exoplanet tentatively identified around the second brightest star in the triple star system Alpha Centauri is accordingly called Alpha Centauri Bb. If an exoplanet orbits both of the stars in a binary system, its name can be, for example, Kepler-34(AB) b.
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The binary nature of the star at the centre of the nebula was discovered in 2014, when a study of why the nebula was not regular was conducted, resolving the previously thought single star into a double star. The two white dwarf stars forming the binary star system at the heart of the nebula orbit each other with a period of about 4 hours. The two stars have a combined mass of about 1.8 solar masses, with each star being slightly less massive than the Sun. As of 2015, they are the most massive binary double white dwarf star system known.
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Located near Alpha is Delta Antliae, a binary star, 450 ± 10 light-years distant from Earth. The primary is a blue- white main sequence star of spectral type B9.5V and magnitude 5.6, and the secondary is a yellow-white main sequence star of spectral type F9Ve and magnitude 9.6. Zeta Antliae is a wide optical double star. The brighter star—Zeta1 Antliae—is 410 ± 40 light-years distant and has a magnitude of 5.74, though it is a true binary star system composed of two white main sequence stars of magnitudes 6.20 and 7.01 that are separated by 8.042 arcseconds.
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Alpha Librae is about from the Sun. The two brightest components of Alpha Librae form a double star moving together through space as common proper motion companions. The brightest member, α2 Librae, is itself a spectroscopic binary system. The second member, α1 Librae, is separated from the primary system by around . It too is a spectroscopic binary with an orbital period of 5,870 days and an angular separation of 0.383 arcseconds; equal to about 10 AU. The system may have a fifth component, the star KU Librae at a separation of 2.6°, thus forming a hierarchical quintuple star system.
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Hercules hosts further quite bright double stars and binary stars. Kappa Herculis is a double star divisible in small amateur telescopes. The primary is a yellow giant of magnitude 5.0, 388 light-years from Earth; the secondary is an orange giant of magnitude 6.3, 470 light-years from Earth. Rho Herculis is a binary star 402 light-years from Earth, divisible in small amateur telescopes. Both components are blue-green giant stars; the primary is magnitude 4.5 and the secondary is magnitude 5.5. 95 Herculis is a binary star divisible in small telescopes, 470 light-years from Earth.
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Optical doubles are so called because the two stars appear close together in the sky as seen from the Earth; they are almost on the same line of sight. Nevertheless, their "doubleness" depends only on this optical effect; the stars themselves are distant from one another and share no physical connection. A double star can be revealed as optical by means of differences in their parallax measurements, proper motions, or radial velocities. Most known double stars have not been studied adequately to determine whether they are optical doubles or doubles physically bound through gravitation into a multiple star system.
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Confirmation of a visual double star as a binary star can be achieved by observing the relative motion of the components. If the motion is part of an orbit, or if the stars have similar radial velocities or the difference in their proper motions is small compared to their common proper motion, the pair is probably physical. When observed over a short period of time, the components of both optical doubles and long-period visual binaries will appear to be moving in straight lines; for this reason, it can be difficult to distinguish between these two possibilities.
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Omega Lupi, Latinized from ω Lupi, is a double star in the southern constellation of Lupus. It is visible to the naked eye with an apparent visual magnitude of 4.33, showing up as a red-hued star just to the south of Gamma Lupi. Based upon an annual parallax shift of 8.97 mas as seen from Earth, it is located around 360 light years from the Sun. As of 2007, the components of this system had an angular separation of 11.4 arc seconds along a position angle of 29°, and are most likely gravitationally bound as a wide binary star system.
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Gamma Cassiopeiae has two faint optical companions, listed in double star catalogues as components B and C. Star B is about 2 arc seconds distant and magnitude 11, and has a similar space velocity to the bright primary. Component C is magnitude 13, nearly an arc second distant. and a further, fainter, optical companion C. Gamma Cassiopeiae A, the bright primary, is itself a spectroscopic binary with an orbital period of about 203.5 days and an eccentricity alternately reported as 0.26 and "near zero." The mass of the companion is believed to be about that of the Sun, but its nature is unclear.
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Giovanni Battista RiccioliAlso "Giambattista" and "Giovambattista" (17 April 1598 – 25 June 1671) was an Italian astronomer and a Catholic priest in the Jesuit order. He is known, among other things, for his experiments with pendulums and with falling bodies, for his discussion of 126 arguments concerning the motion of the Earth, and for introducing the current scheme of lunar nomenclature. He is also widely known for discovering the first double star. He argued that the rotation of the Earth should reveal itself because on a rotating Earth, the ground moves at different speeds at different times.
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After a remake of Escape from New York was announced, Russell was reportedly upset with Gerard Butler for playing his signature character, Snake Plissken, as he believed the character 'was quintessentially [...] American.' Russell appeared in The Battered Bastards of Baseball, a documentary about his father and the Portland Mavericks, which debuted at the Sundance Film Festival in 2014. He co-starred in the action thriller Furious 7 in 2015. On May 4, 2017, Russell and Goldie Hawn received stars in a double star ceremony on the Hollywood Walk of Fame for their achievements in motion pictures, located at 6201 Hollywood Boulevard.
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HD 74389 is a double star system approximately 425 light years from Earth. The primary, HD 74389 A, was initially listed in the Hipparcos catalog as an A0V spectral type star, but this was subsequently updated in 1990 as A2V when Sanduleak and Pesch imaged it with the Burrell Schmidt telescope at Kitt Peak. The primary component is a white A-type main sequence star with an apparent magnitude of +7.48. Its furthest companion, HD 74389 B, is a DA-type white dwarf located 20.11 arcseconds west of—at least 190 AU from—HD 74389 A, and has a V magnitude of 14.62.
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The first well recorded observation of the star system using optical instruments was made by James Bradley on 25 September 1753, when he noticed that it was a double star. William Herschel began systematic observations of 61 Cygni as part of a wider study of binary stars. His observations led to the conclusion that binary stars were separated enough that they would show different movements in parallax over the year, and hoped to use this as a way to measure the distance to the stars. alt=GIF showing the proper motion of the stellar system, taken about in an interval of an year.
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Washington Double Star Catalog) is not explicitly listed, the WGSN says that the name should be understood to be attributed to the brightest component by visual brightness. The WGSN approved the name Almaaz for the brightest component of this system on February 1, 2017 and it is now so included in the List of IAU- approved Star Names. In Chinese, (), meaning Pillars, refers to an asterism consisting of Epsilon Aurigae, Zeta Aurigae, Eta Aurigae, Upsilon Aurigae, Nu Aurigae, Tau Aurigae, Chi Aurigae and 26 Aurigae. Consequently, the Chinese name for Epsilon Aurigae itself is (, "First Star of Pillars").
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The story is set on Tormance, an imaginary planet orbiting the star Arcturus, which, in the novel (but not in reality) is a double star system, consisting of Branchspell, a large yellow sunlike star, and Alppain, a smaller blue star. It is said in the novel to be 100 light- years distant from Earth. There is no systematic description of the geography of Tormance; Maskull simply travels from South to North (with a somewhat eastward excursion to the Sant levels). The direction is symbolic: the light of the second sun, Alppain, is seen to the north; the southern countries are illuminated only by Branchspell.
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HD 43587, being a bright, nearby, high proper motion solar-type star, has been fairly extensively studied. The star was found to be slightly hotter than the Sun, but has a similar metallicity and is therefore not much more massive. Searches for companions to the star, among many other stars, were ongoing throughout the last century. HD 43587 did not seem to have a variable radial velocity or much variability in its astrometry which would indicate that it had a close companion. The Washington Double Star Catalog lists four visual companions; companion B, discovered in 1891, has differing proper motion to the primary, so it is unrelated.
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By 1864 Schur was attending a polytechnic in Hamburg. That summer, he enrolled at the University of Kiel, where he studied mathematics and astronomy under Georg Daniel Eduard Weyer, physics under Gustav Karsten, and philosophy under Friedrich Harms. In the winter semester of 1864/1865 he transferred to the University of Göttingen, where he studied mathematics under Moritz Stern and Karl Hattendorff, physics under Wilhelm Eduard Weber, and astronomy under Wilhelm Klinkerfues, whom Schur was particularly fond of. In April 1867 he published his first astronomical paper, titled "Bahnbestimmung des Doppelsterns Σ 3062" ("Orbit determination of the double star Σ 3062"), in the Astronomische Nachrichten journal.
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An ESO artist's impression of the now-disproven planet Alpha Centauri Bb, orbiting at a distance well short of the star's habitable zone. As one of the brightest stars in Earth's night sky, and the closest-known star system to the Sun, the Alpha Centauri system plays an important role in many fictional works of literature, popular culture, television, and film. Alpha Centauri, a double star system with the binary designation Alpha Centauri AB, is the brightest visible object in the southern constellation Centaurus. Its component stars are Alpha Centauri A (the primary—somewhat larger and brighter than the Sun) and Alpha Centauri B (the secondary—slightly smaller and dimmer).
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As a prominent infrared source, it appears in the Two Micron All-Sky Survey catalogue as 2MASS J16292443-2625549 and the Infrared Astronomical Satellite (IRAS) Sky Survey Atlas catalogue as IRAS 16262–2619. It is also catalogued as a double star WDS J16294-2626 and CCDM J16294-2626. Antares is a variable star and is listed in the General Catalogue of Variable Stars but as a Bayer-designated star it does not have a separate variable star designation. Its traditional name Antares derives from the Ancient Greek , meaning "rival to-Ares" ("opponent to-Mars"), due to the similarity of its reddish hue to the appearance of the planet Mars.
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Its current separation from Fomalhaut A is about , and it is currently located away from TW PsA (Fomalhaut B). LP 876-10 is located well within the tidal radius of the Fomalhaut system, which is . Although LP 876-10 is itself catalogued as a binary star in the Washington Double Star Catalog (called "WSI 138"), there was no sign of a close-in stellar companion in the imaging, spectral, or astrometric data in the Mamajek et al. study. In December 2013, Kennedy et al. reported the discovery of a cold dusty debris disk associated with Fomalhaut C, using infrared images from the Herschel Space Observatory.
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The noted science-fiction writer and critic James Blish was no fan of Heinlein's treatment of his first-person protagonists in a number of his novels. Writing in 1957, however, Blish says that "The only first-person narrator Heinlein has created who is a living, completely independent human being is The Great Lorenzo of Double Star. Lorenzo is complete all the way back to his childhood—the influence of his father upon what he thinks is one of the strongest motives in the story—and his growth under pressure is consistent with his character and no-one else's."James Blish, The Issues at Hand, pp. 53-54.
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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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NGC 2264 including the Cone Nebula and the Christmas Tree Cluster (upside down in this image) with S Monocerotis at the very top of the image (and the base of the Christmas tree) S Monocerotis, also known as 15 Monocerotis, is a massive multiple and variable star system located in the constellation Monoceros. It is the brightest star in the Christmas Tree open cluster in the area catalogued as NGC 2264. S Monocerotis is found within an open cluster and the Washington Double Star Catalog lists many companion stars. The closest and brightest is S Mon B, magnitude 7.8 and 3 arc seconds away.
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Riccioli had come up with 373,000 pedes despite the fact that references to a Roman degree in antiquity had always been 75 milliaria or 375,000 pedes. He is often credited with being one of the first to telescopically observe the star Mizar and note that it was a double star; however, Castelli and Galileo observed it much earlier. In the words of Alfredo Dinis, > Riccioli enjoyed great prestige and great opposition, both in Italy and > abroad, not only as a man of encyclopedic knowledge but also as someone who > could understand and discuss all the relevant issues in cosmology, > observational astronomy, and geography of the time.Dinis 2003 (p. 216).
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Orbital motion has been detected in the central system, but not in the outer pair (as its separation is too high); a preliminary orbit for GG Tauri A has been calculated. Interferometric techniques have been used to observe GG Tauri Ab, the lower- mass component of the central system. GG Tauri Ab may actually be a double star system comprising two red dwarfs (Ab1 = M2V, Ab2 = M3V), with a separation of about 4.5 AU. Its orbital period is currently estimated to be around 16 years. This would explain why the GG Tauri Ab's spectrum suggests an unusually low-mass star instead of the higher mass that was measured.
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Hierarchy of orbits in the Castor system Castor is a multiple star system made up of six individual stars; there are three visual components, all which are spectroscopic binaries. Appearing to the naked eye as a single star, Castor was first recorded as a double star in 1718 by James Pound, but it may have been resolved into at least two sources of light by Cassini as early as 1678. The separation between Castor A and Castor B has increased from about 2″ (2 arcseconds of angular measurement) in 1970 to about 6″ in 2017. These two binary pairs have magnitudes of 1.9 and 3.0.
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By using the HARPS instrument, astronomers detected for the first time a double star where a pulsating Cepheid variable and another star pass in front of one another, which allows to measure the mass of the Cepheid. The study concluded that the mass prediction coming from the theory of stellar pulsation was correct while the value calculated was at odds with the theory of stellar evolution. The discovery of the extrasolar planet Gliese 581 c by the team of Stéphane Udry at University of Geneva's Observatory in Switzerland was announced on April 24, 2007. The team used the telescope's HARPS spectrograph, and employed the radial velocity technique to identify the planet's influence on the star.
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Also a flare star, Proxima has minutes-long outbursts where it brightens by over a magnitude. The Alpha couple revolve in 80-year periodicity and will next appear closest as seen from Earth's telescopes in 2037 and 2038, together as they appear to the naked eye they present the third-brightest "star" in the night sky. One other first magnitude star Beta Centauri is in the constellation in a position beyond Proxima and toward the narrow axis of Crux, thus with Alpha forming a far-south limb of the constellation. Also called Hadar and Agena, it is a double star; the primary is a blue-hued giant star of magnitude 0.6, 525 light-years from Earth.
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Epsilon Chamaeleontis, Latinized from ε Chamaeleontis, is a naked-eye star located in the constellation Chamaeleon and is known as the star HIP 58484, HR 4583, or HD 104174, which during February 1836 Sir John Herschel found as the close double star, HJ 4486AB. Distance is 111±4 pc (362±14 light years) from the Sun, whose absolute magnitude of −0.361 and has the combined visual magnitude of +4.88. Observations throughout the 20th Century have been slowly reducing, whose latest separation is 0.364 arcsec in position angle 211°, as determined on date 1997.0905 using CCD speckle interferometry by E.P. Horch (1997). It is a likely binary system, though no formal orbit has yet been determined.
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It is moving closer to the Earth with a heliocentric radial velocity of −50 km/s, and is predicted to come as near as in around 3.3 million years. This is an aging giant star with a stellar classification of K5 III, having exhausted the supply of hydrogen at its core and expanded to 42 times the Sun's radius. It is radiating 391 times the luminosity of the Sun from its photosphere at an effective temperature of 3,972 K. 56 Aquilae is a double star, but it does not appear to be a binary star system. It is one of the double stars profiled in Admiral William Henry Smyth's 1864 work, Sidereal Chromatics.
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He studied astronomy at the University of Heidelberg and, after the death of his father in 1933, moved to Berlin University. Between 1934 and 1937, he worked as a voluntary at the Berlin-Babelsberg Observatory, which was established by his grandfather Hermann and further developed by his father, and mainly operated the 1.2-meter reflecting telescope which was planned to be built by Hermann. In 1939, shortly after the death of his mother, Wilfried defended his PhD thesis on spectroscopical study of the double star alpha Aurigae (Capella). At the beginning of World War II, Wilfried was enlisted to the infantry at Frankfurt an der Oder and first fought in Poland, France and the Baltic coast of Germany.
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This star was shown to be itself a close double star by S. W. Burnham in 1888, and he discovered an additional 14th-magnitude companion at an angular separation of 31″. Follow on measurements of proper motion showed that Herschel's companion was diverging from Aldebaran, and hence they were not physically connected. However, the companion discovered by Burnham had almost exactly the same proper motion as Aldebaran, suggesting that the two formed a wide binary star system. Working at his private observatory in Tulse Hill, England, in 1864 William Huggins performed the first studies of the spectrum of Aldebaran, where he was able to identify the lines of nine elements, including iron, sodium, calcium, and magnesium.
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The term binary was first used in this context by Sir William Herschel in 1802, when he wrote: By the modern definition, the term binary star is generally restricted to pairs of stars which revolve around a common center of mass. Binary stars which can be resolved with a telescope or interferometric methods are known as visual binaries. For most of the known visual binary stars one whole revolution has not been observed yet, they are observed to have travelled along a curved path or a partial arc. Binary system of two stars The more general term double star is used for pairs of stars which are seen to be close together in the sky.
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This is an aging bright giant star with a stellar classification of G0II. It is a candidate Cepheid variable, but Hipparcos photometry found its brightness to be constant. The star has expanded to 22 times the radius of the Sun and is radiating 283 times the Sun's luminosity from its enlarged photosphere at an effective temperature of 5,051 K. It has a magnitude 13.0 visual companion at an angular separation of along a position angle of 313° relative to the brighter component, as of 2000. HD 102350 is listed in the Washington Double Star Catalog as having a 13th magnitude companion about away, but it is a distant background object unrelated to HD 102350.
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The system is moving closer to the Earth with a heliocentric radial velocity of -24.5 km/s. The two components of 39 Draconis have an angular separation of and take almost 4,000 years to orbit each other. The primary star is an early A-type main-sequence star, having 2.12 times the mass of the Sun with a visual magnitude of 5.06 The secondary is a magnitude 8.07 F-type main-sequence star, and has 1.18 times the mass of the Sun. The 8th-magnitude star HD 238865 is listed in double star catalogues as component C. It is separated from the other two stars by and lies at about the same distance.
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The Catalog of Components of Double and Multiple Stars lists three companions: B is 24 Tauri, a magnitude 6.28 A0 main sequence star 117" away; C is V647 Tauri, a δ Sct variable star; and D is a magnitude 9.15 F3 main sequence star. V647 Tau varies from magnitude +8.25 to +8.30 over 1.13 hours. The Washington Double Star Catalog lists a further four companions, all fainter than 11th magnitude, and also describes component D as itself double with two nearly equal components separated by 0.30". The main star, Alcyone A, consists of three components, the brightest being a blue-white B-type giant similar to many of the other B-type stars in the Pleiades cluster.
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HD 119124 is a wide binary star system in the circumpolar constellation of Ursa Major. With an apparent visual magnitude of 6.3, it lies below the normal brightness limit of stars that are visible with the naked eye under most viewing conditions. An annual parallax shift of 39.24 mas for the A component provides a distance estimate of 83 light years. The pair are candidate members of the Castor Moving Group, which implies a relatively youthful age of around 200 million years. HD 119124 is moving closer to the Sun with a radial velocity of −12 km/s. This system was first identified as a double star by Friedrich von Struve (1793−1864) and catalogued as the 1774th entry in his list.
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The interferometry-measured angular diameter of this star, after correcting for limb darkening, is , which, at its estimated distance, equates to a physical radius of about 16 times the radius of the Sun. τ Sagittarii is a suspected double star although no companion has been confirmed yet. A lower metal content (Fe to H ratio is 54% lower than the sun's) and a high peculiar velocity (64 km/s, four times the local average) relative to the Sun suggest the star is a visitor from a different part of the Galaxy. τ Sagittarii is a red clump giant, a star with similar mass to the sun which has exhausted its core hydrogen, passed through the red giant branch, and started helium fusion in its core.
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It has an optical companion with an apparent magnitude of +6.17 at an angular separation of 0.330 arcseconds and a position angle of 221°, but it is uncertain whether this is an optical double star or a gravitationally bound companion. The star has also been categorized as a spectroscopic binary, indicating that it has an orbiting companion that has not been separately resolved with a telescope. Finally, this star may be a member of the Melotte 20 open cluster, which would make it the second- brightest member after Mirfak. Observation with the IRAS shows an extended, ring-like feature that may be a bow wave driven by radiation pressure from the star, rather than a bubble being generated by the stellar wind.
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In Heidelberg he presented the first stellar-dynamic computations in 1993–1995 of star clusters, in which all stars are born as binary stars. He thus solved the problem that field populations have a significantly lower double star rate than star formation areas, because the binary stars are broken up as the star clusters evolve and disperse. He mathematically formulated and applied a theory of the evolution of binary stars (eigenevolution), created the method of dynamic population synthesis, and predicted the existence of binary stars forbidden by previous theory (forbidden binaries). He suggested in co-operation with Ingo Thies and Christian Theis in 2003–2004 in Kiel that brown dwarves and extrasolar planetary systems can develop in circumstellar disks due to passing stars which disturb the disks.
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Orion's Belt with Alnitak on the left Alnitak has been known since antiquity and, as a component of Orion's belt, has been of widespread cultural significance. It was reported to be a double star by amateur German astronomer George K. Kunowsky in 1819. Much more recently, in 1998, the bright primary was found by a team from the Lowell Observatory to have a close companion; this had been suspected from observations made with the Narrabri Stellar Intensity Interferometer in the 1970s. The stellar parallax derived from observations by the Hipparcos satellite imply a distance around 225 parsecs, but this does not take into account distortions caused by the multiple nature of the system and larger distances have been derived by many authors.
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Omicron Aquilae (ο Aql, ο Aquilae) is the Bayer designation for a double star in the equatorial constellation of Aquila. The brighter component has an apparent visual magnitude of +5.11, which means it is faintly visible to the naked eye in dark suburban skies. The annual parallax shift of this star is 52.11 mas, which is equivalent to a physical distance of from Earth. The primary component, Omicron Aquilae A, is an F-type main sequence star with a stellar classification of F8 V. It has about 125% of the mass of the Sun and 152% of the Sun's radius. With an age of roughly 3.3 billion years, it appears to spinning at a leisurely rate with a projected rotational velocity of 3 km/s.
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The de Sitter double star experiment, later repeated by Brecher under consideration of the extinction theorem. Emission theories, according to which the speed of light depends on the velocity of the source, can conceivably explain the negative outcome of aether drift experiments. It wasn't until the mid-1960s that the constancy of the speed of light was definitively shown by experiment, since in 1965, J. G. Fox showed that the effects of the extinction theorem rendered the results of all experiments previous to that time inconclusive, and therefore compatible with both special relativity and emission theory. More recent experiments have definitely ruled out the emission model: the earliest were those of Filippas and Fox (1964), using moving sources of gamma rays, and Alväger et al.
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According to simple emission theory, light thrown off by an object should move at a speed of c with respect to the emitting object. If there are no complicating dragging effects, the light would then be expected to move at this same speed until it eventually reached an observer. For an object moving directly towards (or away from) the observer at v metres per second, this light would then be expected to still be travelling at (c+v) ( or (c-v) ) metres per second at the time it reached us. In 1913, Willem de Sitter argued that if this was true, a star orbiting in a double-star system would usually, with regard to us, alternate between moving towards us and away from us.
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Pound trained his sister's son, James Bradley, and many of their observations were made together, including the opposition of Mars in 1719, and the transit of Mercury on 29 October 1723. Their measurement of γ Virginis in 1718 was the first made of the components of a double star and was directed towards the determination of stellar parallax. In 1727, Bradley embarked upon a series of observations using a telescope of his own, erected at the rectory in Wanstead, now the site of Wanstead High School. This instrument had the advantage of a large field of view and he was able to obtain precise positions of a large number of stars that transited close to the zenith over the course of about two years.
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A visual binary star is a binary star for which the angular separation between the two components is great enough to permit them to be observed as a double star in a telescope, or even high-powered binoculars. The angular resolution of the telescope is an important factor in the detection of visual binaries, and as better angular resolutions are applied to binary star observations, an increasing number of visual binaries will be detected. The relative brightness of the two stars is also an important factor, as glare from a bright star may make it difficult to detect the presence of a fainter component. The brighter star of a visual binary is the primary star, and the dimmer is considered the secondary.
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Based on parallax measurements from the Hipparcos astrometry satellite, this star is located about from the Earth. It has an apparent visual magnitude of 2.84 and a stellar classification of G5 II. The mass of this star is 3.5 times the mass of the Sun and it is about 240 million years old, which is sufficient time for a star this massive to consume the hydrogen at its core and evolve away from the main sequence, becoming a G-type bright giant. This is a double star system and may be a binary. Using adaptive optics on the AEOS telescope at Haleakala Observatory, the pair was found to be separated by an angle of 2.58 arcseconds at a position angle of 1.4°.
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Like all giant stars, α Cassiopeiae rotates slowly with an approximate velocity of —a speed which takes the star approximately 102 days to make one complete revolution on its axis. Illustration from Gerardus Mercator showing α Cassiopeiae near the heart of the celestial Queen α Cassiopeiae has been sometimes classified as a variable star, but no variability has been detected since the 19th century. Also, three companions to the star have been listed in the Washington Double Star Catalog, but it seems that all of them are just distant line-of-sight optical components. α Cassiopeiae is thought to be around 100 to 200 million years old, having spent much of its time as a blue- white B-type main-sequence star.
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The eclipsing binary pair is separated by only 0.062 astronomical units (au) from each other, whereas the third star in the system (Algol Ab) is at an average distance of 2.69 au from the pair, and the mutual orbital period of the trio is 681 Earth days. The total mass of the system is about 5.8 solar masses, and the mass ratios of Aa1, Aa2, and Ab are about 4.5 to 1 to 2. The three components of the bright triple star used to be, and still sometimes are, referred to as β Per A, B, and C. The Washington Double Star Catalog lists them as Aa1, Aa2, and Ab, with two very faint stars B and C about one arcmin distant.
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Hence it is either a subgiant star around 260 million years old that has nearly exhausted the supply of hydrogen at its core and is in the process of evolving away from the main sequence of stars like the Sun, or a pre main sequence star around 3.2 million years old that has not completely condensed and settled on the main sequence. In 1823, Delta Corvi was found to be a wide double star by British astronomers James South and John Herschel. Since that time, the position of the two stars with respect to each other has not changed. The magnitude 9.3 companion, HR 4757 B, with a classification of K2Ve, is at an angular separation of 24.2 arcseconds along a position angle of 214°.
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Having exhausted the supply of hydrogen at its core, the star has cooled and expanded off the main sequence, and now has over seven times the girth of the Sun. It is radiating 24 times the luminosity of the Sun from its swollen photosphere at an effective temperature of 4,824 K. The secondary is a magnitude 10.24 star at an angular separation of from the primary along a position angle of 2°, as of 2015. The Washington Double Star Catalog (2001) notes this is an "optical pair, based on study of relative motion of the components," whereas Eggleton and Tokovinin (2008) list it as a binary system. Gaia Data Release 2 gives a parallax of for the companion, implying a distance around .
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Many of the most enduring science fiction tropes were established in Golden Age literature. Space opera came to prominence with the works of E. E. "Doc" Smith; Isaac Asimov established the canonical Three Laws of Robotics beginning with the 1941 short story "Runaround"; the same period saw the writing of genre classics such as the Asimov's Foundation and Smith's Lensman series. Another frequent characteristic of Golden Age science fiction is the celebration of scientific achievement and the sense of wonder; Asimov's short story "Nightfall" exemplifies this, as in a single night a planet's civilization is overwhelmed by the revelation of the vastness of the universe. Robert A. Heinlein's 1950s novels, such as The Puppet Masters, Double Star, and Starship Troopers, express the libertarian ideology that runs through much of Golden Age science fiction.
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Avoiding Bolt, the law, and an incited mob convinced the children are witches, they eventually make their way up Witch Mountain, pursued by Deranian and Ubermann, as well as by Bolt in a helicopter. As their memories begin to fully return, the children realize their accident at sea did not involve a boat but a spacecraft. Tony and Tia are actually of extraterrestrial origin; the double star emblem on the star case stands for a binary star system where their home planet was located. Having come to Earth because their own planet was dying, survivors of the journey made their way to Witch Mountain and formed a community to await the surviving children, each pair in possession of a star case to help them find their way to their new home.
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Delta Corvi, traditionally called Algorab, is a double star divisible in small amateur telescopes. The primary is a blue-white star of magnitude 2.9, around 87 light-years from Earth. An enigmatic star around 2.7 times as massive as the Sun, it is more luminous (65–70 times that of the Sun) than its should be for its surface temperature of 10,400 K, and hence is either a 3.2 million year-old very young pre-main sequence star that has not settled down to a stable main sequence life stage, or a 260-million-year-old star that has begun to exhaust its core hydrogen and expand, cool and shine more brightly as it moves away from the main sequence. Its spectral type is given as A0IV, corresponding with the latter scenario.
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Sigma Tauri (σ Tauri) is the Bayer designation for a pair of white-hued stars in the zodiac constellation of Taurus. The system is a visual double star, whose components are designated σ1 Tauri and σ2 Tauri, with the latter being the more northerly star. The two are separated by 7.2 arcminutes on the sky and can be readily split with a pair of binoculars. They have apparent visual magnitudes of +5.07 and +4.70, respectively, which indicated they are both visible to the naked eye. Based upon parallax measurements, σ1 Tauri is about 147 light years from the Sun, while σ2 Tauri is 156 light years distant. σ1 Tauri is a single-lined spectroscopic binary star system with an orbital period of 38.951 days and an eccentricity of 0.15.
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Delta Cancri (δ Cancri, abbreviated Delta Cnc, δ Cnc) is a double star about 180 light-years from the Sun in the constellation of Cancer. Its two main constituents are designated Delta Cancri A and B. A is itself a binary star whose components are Delta Cancri Aa (formally named Asellus Australis , the traditional name of the entire system) and Ab. The star system is 0.08 degree north of the ecliptic, so it can be occulted by the Moon and more rarely by planets; it is occulted (eclipsed) by the sun from about 31 July to 2 August.In the Sky Earth astronomy reference utility showing the ecliptic and relevant date as at J2000 - present Thus the star can be viewed the whole night, crossing the sky at the start of February.
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Caelum is a faint constellation: It has no star brighter than magnitude 4 and only two stars brighter than magnitude 5\. Lacaille gave six stars Bayer designations, labeling them Alpha (α ) to Zeta (ζ ) in 1756, but omitted Epsilon (ε ) and designated two adjacent stars as Gamma (γ ). Bode extended the designations to Rho (ρ ) for other stars, but most of these have fallen out of use. Caelum is too far south for any of its stars to bear Flamsteed designations. The constellation Caelum as it can be seen by the alt=Image of the constellation Caelum, showing the pattern of its stars as seen in the night sky The brightest star, (Alpha) α Caeli, is a double star, containing an F-type main-sequence star of magnitude 4.45 and a red dwarf of magnitude 12.5 , from Earth.
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The bogies are a monomoteur design,Monomoteur (English: mono-motor or single motor) - a single (2.8MW) electric motor is mounted in the bogie and drives both axles with helical spring primarily suspension. The traction motors are three phase synchronous type (as used in the contemporary TGV Atlantique) but with two three phase stator windings offset by 30 degrees.A "double star" (French: double étoile) type with 12 pole elements was used for the BB 26000 locomotives, whereas the single three phase motors used in the TGV Atlantique had only 6 stator poles set 60 degrees apart Drive from the traction motors to wheel is via a floating ring vibration isolation element (French:anneau dansant) and hollow shaft drive. Mono-motor bogies were chosen based on the good performance in the SNCF BB 22200, SNCF BB 15000 and SNCF BB 7200 classes.
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Pulkovo Observatory in 1839. During 1843 and 1844, Struve participated in longitude measurements between Altona, Greenwich and Pulkovo, which were based on large displacement of chronometers over the Earth surface. This newly developed method was adopted in Russia, and from 1844, the longitude was measured starting not from the Tartu Observatory but from the Pulkovo Observatory. Much of the 1844 Struve dedicated to studying the Sun. He deduced its apex coordinates and linear velocity as 7.3 km/s. Although it was significantly smaller than the correct value of 19.5 km/s measured in 1901, Struve's result was correct in that the velocity of the Sun was smaller than that of stars. In 1865 he discovered NGC 8, a double star in the constellation Pegasus. This occurred only 2 days after he discovered the spiral galaxy NGC 9 in the constellation Andromeda.
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After Michell's death in 1793, Herschel bought a ten-foot-long, 30-inch reflecting telescope from Michell's estate. In 1797, Herschel measured many of the systems again, and discovered changes in their relative positions that could not be attributed to the parallax caused by the Earth's orbit. He waited until 1802 (in Catalogue of 500 new Nebulae, nebulous Stars, planetary Nebulae, and Clusters of Stars; with Remarks on the Construction of the Heavens) to announce the hypothesis that the two stars might be "binary sidereal systems" orbiting under mutual gravitational attraction, a hypothesis he confirmed in 1803 in his Account of the Changes that have happened, during the last Twenty- five Years, in the relative Situation of Double-stars; with an Investigation of the Cause to which they are owing. In all, Herschel discovered over 800 confirmedWilliam Herschel's Double Star Catalog. Handprint.
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The AMS-IX platform is continually evolving due to its rapid growth in traffic and number of connected member ports. Up until end of 2009, it is using a redundant hub- spoke architecture using a core switch and multiple edge switches. This double-star topology brings the advantage of being able to perform maintenance on the network without any impact on customer traffic, and to anticipate on fiber and equipment problems by (automatically) switching to the backup topology as soon as a failure in one of the active components occurs. The active switching topology star is determined by means of the VSRP protocol. This topology is AMS-IX version 3. However, since 2009; AMS-IX platform has migrated from a pure Layer2 network to a VPLS/MPLS network (using Brocade hardware) in order to cope with future growth (this is AMS-IX version 4).
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2nd seeded Nehwal beat Sung Ji-hyun of South Korea 21–13, 21–14 to win the Swiss Open title. Nehwal faltered after a good start as she lost to the then world number three Wang Xin of China in the finals to finish runner-up in the 2011 Malaysian Open tournament. She was a part of Indian Team in the 2011 BWF Double Star Sudirman Cup mixed team who managed to reach the quarterfinals of this elite mixed team event for the first time ever, as India managed to beat Thailand 3–2, even when Saina lost her tie against Ratchanok Intanon. In the quarterfinals against China, Nehwal put up her best performance and beat the then world number two Wang Xin with 21–15, 21–11, but still the Chinese managed to move into the semi finals with a 3–1 win over India.
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Pound's observations with it of the five known satellites of Saturn enabled Halley to correct their movements; and Newton employed, in the third edition of the Principia, his micrometrical measures of Jupiter's disc, of Saturn's disc and ring, and of the elongations of their satellites; and obtained from him data for correcting the places of the comet of 1680. Laplace also used Pound's observations of Jupiter's satellites for the determination of the planet's mass; and Pound himself compiled in 1719 a set of tables for the first satellite, into which he introduced an equation for the transmission of light. Pound trained his sister's son, James Bradley, and many of their observations were made together, including the opposition of Mars in 1719, and the transit of Mercury on 29 October 1723. Their measurement of γ Virginis in 1718 was the first made of the components of a double star and was directed towards the determination of stellar parallax.
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Though there are some sources indicating that the star is a spectroscopic binary, including the Washington Double Star Catalog (WDS) and the Gliese Catalogue of Nearby Stars, no orbit has been provided. The WDS lists four companions to Rho Geminorum. Of these, surprisingly little is known about the closest companion, the magnitude 12.5 Rho Geminorum B. The most recent measurement lists a separation of 3.4 arcseconds, corresponding to a separation perpendicular to the line of sight of approximately 85 AU. The spectral type listed in SIMBAD is M5, though this is without a source; Plotting the star's absolute magnitude on the Hertzsprung-Russell diagram (see left) indicates a B-V of 1.53, a value closer to that of an M3V star. Peculiarly, the five observations recorded in the WDS date between 1910 and 1935 and none have been made since; even in literature, more recent attempts to resolve Rho Geminorum B have been unsuccessful.
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The Vigilantes did not carry on the name of Dallas' previous AFL team, the Dallas Desperados, because of a unique ownership situation with the former team. Although the new AFL owns the former AFL team assets (hence the Arizona Rattlers, Chicago Rush, Cleveland Gladiators, Orlando Predators, Tampa Bay Storm, and Utah Blaze names going over to the new AF1), former Desperados owner Jerry Jones (who also owns the NFL's Dallas Cowboys) retained the team's branding rights after it folded. Jones had based most of the Desperados branding on that of the Cowboys, including the colors, prominent use of a star in the logo, and a Cowboys "Double Star" logo on the front of the Desperados' jerseys, thus making the Cowboys and Desperados branding very difficult to separate. Not willing to risk such complicated legal action, and apparently unwilling to revive the Fort Worth Cavalry (another former AFL team that played in the region that coincidentally was owned by Kern), the Vigilantes chose a new name.
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HR 5171 was named by inclusion in the Harvard Revised catalogue, later published as the Bright Star Catalogue. It was the 5171th entry in the catalogue, listed with a visual magnitude of 6.23 and K-type spectral type. HR 5171 was catalogued as a double star in 1927. In 1956, HR 5171 was recorded at magnitude 6.4, spectral type G5p, and profoundly reddened. In 1966 Corben recorded it as magnitude 6.51 and spectral type G5p, and noted it as being variable. A 1969 catalogue records a visual magnitude of 5.85 and a spectral type of A7V, presumably a case of mistaken identity. In 1971, HR 5171 A was identified as a G8 hypergiant, reddened by over three magnitudes of interstellar extinction and also by half a magnitude of extinction from circumstellar material. In 1979 it was confirmed as one of the brightest known stars with an absolute visual magnitude (MV) of −9.2.
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Orbital path of Robert Heinlein's eponymous asteroid In his lifetime, Heinlein received four Hugo Awards, for Double Star, Starship Troopers, Stranger in a Strange Land, and The Moon Is a Harsh Mistress, and was nominated for four Nebula Awards, for Stranger in a Strange Land, Friday, Time Enough for Love, and Job: A Comedy of Justice. He was also given seven Retro-Hugos: two for best novel: "Beyond This Horizon" and "Farmer in the Sky"; Three for best novella: :"If This Goes On ...", "Waldo", and "The Man Who Sold the Moon"; one for best novelette: "The Roads Must Roll"; and one for best dramatic presentation: "Destination Moon". Heinlein was also nominated for six Hugo Awards: Have Space Suit - Will Travel, Glory Road, Time Enough for Love, Friday, Job: A Comedy of Justice, Grumbles from the Grave; and six Retro Hugo Awards: Magic, Inc., "Requiem", "Coventry", "Blowups Happen", "Goldfish Bowl", "The Unpleasant Profession of Jonathan Hoag".
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The Vigilantes did not carry on the name of Dallas' previous AFL team, the Dallas Desperados, because of a unique ownership situation with the former team. Although the new AFL owns the former AFL team assets (hence the Arizona Rattlers, Chicago Rush, Cleveland Gladiators, Orlando Predators, Tampa Bay Storm, and Utah Blaze names going over to the new AF1), former Desperados owner Jerry Jones (who also owns the NFL's Dallas Cowboys) retained the team's branding rights after it folded. Jones had based most of the Desperados branding on that of the Cowboys, including the colors, prominent use of a star in the logo, and a Cowboys "Double Star" logo on the front of the Desperados' jerseys, thus making the Cowboys and Desperados branding very difficult to separate. Not willing to risk such complicated legal action, and apparently unwilling to revive the Fort Worth Cavalry (another former AFL team that played in the region that coincidentally was owned by Kern), the Vigilantes chose a new name.
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It was a modern high wing monoplane with a wooden structure and canvas covering, equipped with a wing warping system to control the roll and reinforced by metal tie rods connected to the fuselage and to a special structure placed above it; the fuselage was based on a wooden lattice structure, in turn reinforced by metal cables, and was covered in cloth only for the front half; the same wooden structure with a canvas covering characterized the empennages. The trolley, fixed, was composed of two front wheels with anti-overblank pads and another smaller, tailed shoe. The Ca.12 differed from its immediate predecessors mainly due to the fact of being a two-seater, with the two cockpits arranged "in tandem" (ie one behind the other); moreover, the Ca.12 differed from the Ca.11 for the greatly enlarged wing opening and for the engine, a radial Anzani 6A3 6- cylinder double star capable of developing a power of 60 hp. Other versions of the same model were powered by 50 or 70 HP engines.
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Moreover, he is recognized as the first Spanish in calculating the orbit of a double star system in the country, the STT 77. It follows the appointment of Aller as a member of the “International Astronomical Union Commission 26 (double stars)” in 1948 (Zurich). The following year he was named a member of the National Commission on Astronomy. The professor Aller Ulloa also designed and built devices for measuring and observation purchased by the Paris Observatory; he suggested modifications on the production of the astrograph to the German manufacture Zeiss, which accepted them and afterwards did not accept the payment of Aller Ulloa for the device as appreciation for the improvements; a clock of sidereal time; a base for the portable vertical circle monocular, etc..."Ramón María Aller Ulloa" Contistuted by his two main research lines double stars and the methods to determine coordinates based on two vertical lanes he published 78 articles in especialized publications in Europe, 4 books and he directed 5 PhD thesis (Between 1960 and 1963, in spite of being 83 years old, Aller still directed three theses: Múgica Buhigas's “ber die Anwendung des Theodolits in der Geodtischen Astronomia” (Munich, 1960); Zaera de Toledo's “On determining the Orbits of Visual Double Stars.
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