How about if this binary star system is orbiting another binary star system?
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Well, binary star systems are stable, so let's start there.
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A binary star system with Harden turned into a black hole.
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She's the author of one previous book, the novel "Binary Star" (2015).
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Due to movement, the binary star system wasn't observed by OGLE in 2005.
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This is possible in a binary star system, in which two stars orbit each other.
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This star was found as an almost invisible secondary star in a binary star system.
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Zellem later observed the first planet found to orbit a binary star system, Kepler-16b.
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Also in the great beyond, in the constellation Aquarius, lies a binary star called R Aquarii.
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It's one of two stars in a binary star system, partnered with a red dwarf star.
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But the two neutron stars that collided are more massive than all known binary star pairs.
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And this binary-star system is one of the best characterized yet due to its eclipsing nature.
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TESS measurements of the binary star system helped astronomers discover the mutual eclipses and rule out pulsating.
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More realistically, 'Oumuamua was tossed from a hot, nascent binary star system still in its planet-making mode.
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Normally, a protoplanetary disk rests along the same plane as the orbital plane of its binary star hosts.
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More specifically, they were looking for binary star systems that could be used to better determine astronomical distances.
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In systems with multiple planets orbiting the same binary star system, "even wilder things can happen," he continued.
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The binary star system, where the stars are around a billion years old, is known as BD + 20 307.
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The exponent indicates the presence of a binary star system, so yes, this star has a companion named π2 Gruis.
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Scientists have never seen a binary star system in the midst of forming, but capture is given as one potential mechanism.
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Astronomers have now identified the source of that brief brightening — a binary star system a couple of thousand light-years away.
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That image was a mental stand-in for the prediction of planets orbiting a binary star system before the detection was made.
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The telescope high in the desert of Chile captured images of IRAS 16400-2422, a binary star system some 400 light years away.
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They studied the binary star system, HD101584, using the Atacama Large Millimeter/submillimeter Array of telescopes in Chile to find out what happened.
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A type 1a supernova is a binary star in which a small, dense object called a white dwarf pulls material from a larger companion.
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The inset depicts the debris disk surrounding IRAS 08544-4431, a binary star buried in the Vela constellation some 4,000 light years from home.
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While Breakthrough Starshot was initially packaged as a voyage to the nearby binary star system Alpha Centauri, the discovery of Proxima b changes everything.
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And when the first "Star Wars" film was made, astronomers had yet to discover a planet in the universe within a binary star system.
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This week, the Chandra X-ray Observatory followed developments within IC 10, a starburst galaxy with more than a dozen x-ray binary star systems.
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A mere 8,000 light years away in our home galaxy is another black hole, this one part of a binary star system called V404 Cygni.
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One idea that they float is Mission Centaur, a small space telescope designed to locate any Earth-like planets discovered around the binary star system.
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After years of searching, their modern counterparts identified the source of that brief brightening — a binary star system a couple of thousand light-years away.
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Her first, "Binary Star," a novel about a pair of lost 20-somethings falling out of love, was praised for its intensity and simple prose.
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Perhaps it came from a binary star system, or a system with a giant planet, either of which could have launched the object into interstellar space.
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It takes place once every 69 years in the binary star system TYC 6723-672-1 and lasts for approximately three and a half Earth-years.
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On March 6th, the European Southern Observatory (ESO) posted a mesmerizing image of a binary star system, captured by the agency's Atacama Large Millimeter/submillimeter Array (ALMA).
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"The orientation of this binary star system created a fantastic cosmic laboratory," said Scott Ransom, study co-author and an astronomer at the National Radio Astronomy Observatory.
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New research suggests this visitor from afar likely came from a binary star system, and that astronomers should be on the lookout for both interstellar asteroids and comets.
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The galaxies contain numerous high-mass X-ray binary star systems, captured in a composite image with data from NASA's Chandra Observatory, NuStar, and the Hubble Space Telescope.
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They have also spotted similar binary star systems that appear quite stable, calmly orbiting each other, and others that are belching only small eruptions known as dwarf novas.
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Read These Stories Next:Meet Billions' Asia Kate Dillon, TV's First Non-Binary Star Where We Left Off With The Very Luxe Billions Inside Our Fascination With The Filthy Rich
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This binary star system and its planets represents the smallest-separation twin binary, where both stars host planets, that has ever been observed, according to lead researcher Johanna Teske.
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More than half of those, in turn, exist in binary star systems that have also been disregarded as being too different from the conditions present in the solar system.
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" Binary star systems are two stars that orbit around each other, not unlike the twin suns we see in the sky over Tatooine in "Star Wars: A New Hope.
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That's all good—but scientists have come to the realization that a particular light source, one assumed to be binary star system in Andromeda, may actually be something far stranger.
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Most telescopes have a way of getting around the brightness of stars blocking the view of orbiting bodies, but most don't account for a binary star system like Alpha Centauri.
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Image: J. Skowron, K. Ulaczyk / Warsaw University ObservatoryIn 2009, a binary star that had been flaring up for years suddenly exploded, growing millions of times brighter in a cosmic blink.
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NASA wants you to work on Mars Proxima Centauri coexists with a binary star in Alpha Centauri, a well-studied star system that serves as a neighbor to our sun.
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In 2005, the Very Large Telescope was studying a potential exoplanet that happened to be in the same vicinity as V1213 Cen, a binary star system in the Centaurus constellation.
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And, at just 8,000 light years from the Earth in our own Milky Way galaxy, is a black hole that is part of a binary star system called V404 Cygni.
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Thanks to NASA's Kepler space telescope, which was created with the goal of taking a census of our galactic neighbourhood, we now know of several planets orbiting binary star systems.
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The new image, released by the European Southern Observatory (ESO) on Wednesday, captures the aftermath of a confrontation inside a binary star system called HD101584, located thousands of light years from Earth.
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"This is the first evidence of frame-dragging in a binary star system," said lead author Vivek Venkatraman Krishnan, a physicist at the Max Planck Institute for Radio Astronomy, in an email.
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He was pointing out that the waves from a typical binary star system would carry away so little energy, we would never even notice that the system had changed—and that is true.
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The planets that researchers have turned up range from big and weird — like a Jupiter-sized planet orbiting a binary star system — to ones that are closer in size and orbit to Earth.
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Check out this mesmerizing animation of the binary star system AR Scorpii, in which a white dwarf repeatedly thrashes its red dwarf partner with jets of radiation, causing regular pulses every 1.97 minutes.
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To that point, Reitze said that LIGO is likely to pick up on gravitational waves from predicted sources like black hole mergers, binary star systems, supernovae, and other phenomenon within the next year.
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For example, it found a simple form of sugar in the gas surrounding a young binary star, demonstrating that some of the chemical foundations of life on Earth also exist in faraway galaxies.
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Most star systems involve blazingly hot and massive gas giants that sit uncomfortably close to their host stars, or binary star systems in which complex gravitational effects make it difficult for planets to form.
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"My co-authors and I have a bet against a couple people studying binary star formation that within the first 100 LIGO detections, LIGO will detect something within this upper mass gap," Rodriguez said.
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Image: University of Warwick/Mark GarlickAstronomers using the ALMA telescope have discovered an oddly tilted planet-forming disk within a double binary star system, a configuration that up until this point only existed in theory.
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A planet orbiting a young binary star system might have been disturbed by another pair of stars that came too close about 2 million to 23 million years ago, soon after the planet was formed.
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Each member of the binary star pair would be almost as bright as the full moon, though without a good telescope they would look like dots of light about a pinky-finger-width apart in the sky.
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"We discovered this binary star merger two years ago, and it was close to the Milky Way—much closer than we anticipated," Imre Bartos, the study's first author and assistant professor at the University of Florida, told Gizmodo.
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According to previous studies, binary star systems that drift too close to the black hole could be torn apart by strong tidal forces, resulting in one star being consumed while the other is drop-kicked out of the galaxy.
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As it turns out, Kepler has discovered key insights about the unique nature of our stellar neighborhood, which have included blazing-hot gas giants in perilous proximity to their host stars, binary star systems, and red dwarfs orbited by numerous rocky worlds.
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One such idea began brewing in 2014, when de Mink and Ilya Mandel, an astrophysicist at the University of Birmingham and a member of the LIGO collaboration, realized that a type of binary-star system that de Mink has studied for years might be just the ticket to forming massive binary black holes.
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HD 153370 is binary star in the southern constellation of Ara.
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Schematic of a binary star system with one planet on an S-type orbit and one on a P-type orbit. Planets in binary star systems may be candidates for supporting extraterrestrial life. Habitability of binary star systems is determined by many factors from a variety of sources. Typical estimates often suggest that 50% or more of all star systems are binary systems.
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HD 118889 is a binary star in the northern constellation of Boötes.
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HD 149837 is a binary star in the southern constellation of Ara.
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HD 165259 is visual binary star system in the southern constellation of Apus.
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S Antliae is a W Ursae Majoris-type eclipsing binary star in Antlia.
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HD 127726 is a binary star system in the northern constellation of Boötes.
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HD 216718 is a binary star system in the equatorial constellation of Aquarius.
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HD 174569 is a spectroscopic binary star system in the equatorial constellation of Aquila.
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HD 112028 and HD 112014 together are known as the binary star Struve 1694.
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Some planets orbit one member of a binary star system,Schwarz, Richard. Binary Catalogue of Exoplanets. Universität Wien and several circumbinary planets have been discovered which orbit around both members of binary star. A few planets in triple star systems are knownSchwarz, Richard. STAR-DATA.
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HD 77258 is a spectroscopic binary star in the constellation Vela. Its apparent magnitude is 4.47.
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Using this same principle, Jalowiczor searched for planets orbiting a star, instead of binary star systems.
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Here he met Senim Silla, and they formed the rap group Binary Star while in prison.
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HD 109749 is a binary star about 206 light years away in the constellation of Centaurus.
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Kepler-89 is a star with four confirmed planets. Kepler-89 is a possible wide binary star.
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The Name, The Motto, The Outcome is the only solo album from Binary Star member Senim Silla.
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UU Aurigae is a carbon star and binary star in the constellation Auriga. It is approximately from Earth.
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HD 93250 is a highly luminous hot blue binary star in the Carina Nebula in the constellation Carina.
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HD 164509 is a binary star system composed of two main sequence stars in the constellation of Ophiuchus.
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It figures directly between Alpha and Beta. Indus is home to one bright binary star. Theta Indi is a binary star divisible in small amateur telescopes, 97 light-years from Earth. Its primary is a white star of magnitude 4.5 and its secondary is a white star of magnitude 7.0.
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HD 38529 (138 G. Orionis) is a binary star approximately 138 light-years away in the constellation of Orion.
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Gamma Herculis, Latinized from γ Herculis, is a magnitude 3.74 binary star system in the northern constellation of Hercules.
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Nu Capricorni (ν Capricorni, abbreviated Nu Cap, ν Cap) is a binary star in the southern constellation of Capricornus.
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HD 49798 is binary star in the constellation Puppis about 650 parsecs from Earth. It has an apparent magnitude of 8.3. HD 49798 was discovered in 1964 to be a rare hydrogen-deficient O class subdwarf. This was identified as a binary star, but the companion could not be detected visually or spectrscopically.
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Recent measurements indicate that the binary star system has an age of several billion years -- comparable to the Solar System.
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From 2013 to 2015 he also hosted a weekly podcast "Foreallyshow" with childhood friend, rapper Senim Silla of Binary Star.
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9 Sagittarii (9 Sgr) is a massive binary star in the constellation Sagittarius. It has an apparent magnitude of 5.97.
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Nu3 Canis Majoris, Latinized from ν3 Canis Majoris, is a binary star system in the southern constellation of Canis Major.
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An eclipsing binary star is a binary star system in which the orbit plane of the two stars lies so nearly in the line of sight of the observer that the components undergo mutual eclipses. In the case where the binary is also a spectroscopic binary and the parallax of the system is known, the binary is quite valuable for stellar analysis. Algol, a triple star system in the constellation Perseus, contains the best-known example of an eclipsing binary. This video shows an artist's impression of an eclipsing binary star system.
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W Cygni has been proposed as a binary star with a hotter main sequence companion, but it has not been confirmed.
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A symbiotic binary star is a variable binary star system in which a red giant has expanded its outer envelope and is shedding mass quickly, and another hot star (often a white dwarf) is ionizing the gas. Three symbiotic binaries as of 1999 are SSXSs: AG Dra (BB, MW), RR Tel (WD, MW), and RX J0048.4-7332 (WD, SMC).
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The secondary, 30 Cygni, appears blue-green. It is of spectral type A5IIIn and magnitude 4.83, and is around 610 light-years from Earth. 31 Cygni itself is a binary star; the tertiary component is a blue star of magnitude 7.0. Psi Cygni is a binary star visible in small amateur telescopes, with two white components.
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Others are the result of mass transfer in a binary star system; examples of these include the barium stars and some S stars.
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LH54-425 is a spectroscopic binary star system in the LH 54 OB association within the Large Magellanic Cloud in the constellation Dorado.
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The peculiarities in the LMC stars may be due to binary interactions, although κ Pav is not known to be a binary star.
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HD 200375 is a binary star system in the equatorial constellation of Aquarius. Their orbit does not yet have a unique solution available.
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However, as the mass of the companion is greater than 2.8 solar masses, this strongly suggests this companion is itself a binary star.
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Pi Aquarii, Latinized from π Aquarii, is the Bayer designation for a binary star in the equatorial constellation of Aquarius. This system has an apparent visual magnitude of a mean apparent magnitude of +4.57. Based upon parallax measurements, it is located at a distance of roughly from Earth. This is a binary star system with an orbital period of 84.1 days.
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DT Virginis, also known as Ross 458 AB, is a binary star in the constellation of Virgo. Both of the stars are low-mass red dwarfs with at least one of them being a flare star. This binary system has a circumbinary planet detected by direct imaging, currently the planetary-mass object with the widest known orbit around a binary star.
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Upsilon4 Eridani is a close binary star system in the constellation Eridanus. It is visible to the naked eye with an apparent visual magnitude of 3.56. Based upon parallax measurements, the pair are located around from the Sun. This is a double-lined spectroscopic binary star system, which means that the Doppler-shifted spectral lines of both components can be distinguished.
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Mu Eridani (μ Eridani) is a binary star system in the constellation Eridanus. It is visible to the naked eye with an apparent visual magnitude of 4.00. Based upon an annual parallax shift of 0.00625 arcseconds, it is located roughly 520 light years from the Sun. In 1910, this was determined to be a single-lined spectroscopic binary star system.
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Xi Cephei is another binary star, 102 light-years from Earth, with a period of 4,000 years. It has a blue-white primary of magnitude 4.4 and a yellow secondary of magnitude 6.5. Kruger 60 is an 11th-magnitude binary star consisting of two red dwarfs. The star system is one of the nearest, being only 13 light-years away from Earth.
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The primary component of the binary star system, 2MASS J18082002−5104378 A, is a subgiant, cooler than the Sun, but larger and more luminous.
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HD 134064 is a binary star system in the northern constellation of Boötes. The pair are separated by a distance of around 8,000 AU.
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HD 31093 (also known as HIP 22573) is a binary star system in the constellation Caelum. HD 31093 is roughly 268 light years distant.
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HD 214810 is a visual binary star in the equatorial constellation of Aquarius. The pair orbit each other with a period of about 54.2 years.
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HD 87822 is a binary star in the northern constellation of Leo Minor. The pair orbit each other with a period of about 18 years.
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Epsilon Ceti, Latinized from ε Ceti, is the Bayer designation for a binary star system located in the equatorial constellation of Cetus. It is faintly visible to the naked eye with an apparent visual magnitude of +4.84. Based upon an annual parallax shift of 14.58 mas, it is located around 98 light years away from the Sun. This is a line-width spectroscopic binary star system.
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1 Persei (1 Per) is an eclipsing binary star in the constellation Perseus. Its uneclipsed apparent magnitude is 5.49. The binary star consists of two B2 type main-sequence stars in a 25.9 day eccentric orbit. The stars are surrounded by a faint cloud of gas visible in mid-infrared, although whether they are the origin of the gas or simply passing through it is unclear.
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Kruger 60 (DO Cephei) is a binary star system located 13.15 light-years from the Sun. These red dwarf stars orbit each other every 44.6 years.
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Kepler-432 is a binary star system with at least two planets in orbit around the primary companion, located about 2,830 light-years away from Earth.
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The two stars do not form a binary star system as 35 Leo is only 100 light years from Earth, thus separating the two stars by approximately .
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Alpha Ophiuchi (α Ophiuchi, abbreviated Alpha Oph, α Oph), also named Rasalhague ,also or . is a binary star and the brightest star in the constellation of Ophiuchus.
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TU Muscae, also known as HD100213, is an eclipsing binary star in the constellation Musca. Its apparent magnitude ranges from 8.17 to 8.75 over around 1.4 days.
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Pi4 Orionis (π4 Ori, π4 Orionis) is a binary star system in the western part of the Orion constellation. It is visible to the naked eye with an apparent visual magnitude of 3.7. Based upon an annual parallax shift of 3.1 mass, it is located roughly 1,050 light years from the Sun. This is a spectroscopic binary star system with an orbital period of 9.5 days and an eccentricity of 0.03.
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Psi6 Aurigae, Latinized from ψ6 Aurigae, is a spectroscopic binary star in the northern constellation of Auriga. It is a dim, naked eye star with an apparent visual magnitude of +5.22. Based upon a measured annual parallax shift of , it is approximately distant from the Earth. This is a single-lined spectroscopic binary star system with an orbital period of 5,996 days (16.4 years) and an eccentricity of 0.044.
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Other common examples are the orbit of a moon around a planet, and of a planet around a star, and two stars orbiting each other (a binary star).
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HD 188405 is a binary star in the equatorial constellation of Aquila. The pair have an orbital period of roughly 425 years and an angular separation of 1.085″.
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BB Doradus or BB Dor is a cataclysmic variable or nova-like star that is a binary star system composed of a red dwarf and a white dwarf.
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Three blue stragglers have been detected in the cluster and at least three red giants are indisputable members of the cluster, one of which being a spectroscopic binary star.
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Alpha Pavonis (α Pavonis, abbreviated Alpha Pav, α Pav), formally named Peacock , is a binary star in the southern constellation of Pavo, near the border with the constellation Telescopium.
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7 Vulpeculae is a binary star system approximately 940 light years away in the northern constellation of Vulpecula. It is a challenge to view with the naked eye, having an apparent visual magnitude of 6.33. The system is moving closer to the Earth with a heliocentric radial velocity of −38 km/s. This is a single-lined spectroscopic binary star system with an orbital period of 69.3 days and an eccentricity of 0.16.
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Beta Muscae, Latinized from β Muscae, is a binary star in the southern circumpolar constellation of Musca. With a combined apparent visual magnitude of 3.07, it is the second brightest star (or star system) in the constellation. Judging by the parallax results, it is located at a distance of roughly from the Earth. This is a binary star system with a period of about 194 years at an orbital eccentricity of 0.6.
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Tau8 Eridani, Latinized from τ8 Eridani, is a binary star system in the constellation Eridanus. It is visible to the naked eye with a combined apparent visual magnitude of 4.65. The distance to this system can be estimated via the parallax method, yielding a value of around 380 light years. This is a single-lined spectroscopic binary star system with an orbital period of about 459 days and an eccentricity of 0.18.
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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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R145 (HD 269928) is a spectroscopic binary star in the Tarantula Nebula in the Large Magellanic Cloud located in the constellation Dorado. Both components are amongst the most luminous known.
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Most likely the pair form a binary star system. At least one of the stars appears to be a source of X-ray emission. The X-ray band flux is .
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The faint OIII ring structure can be seen through a telescope. The central star of Abell 70 is a binary star consisting of a white dwarf and a barium star.
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He has delivered the keynote talk at the Conference for Underrepresented Minority Physicists (CU2MiP). His current work focuses on extreme ultraviolet laser light and spectroscopic analysis of binary star systems.
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There is a visual companion, CCDM J23186+6807C, to the binary star. It has an approximate apparent visual magnitude of 12.8 and is located approximately 45 arcseconds away from it.
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Kappa Crucis (κ Cru, HD 111973) is a spectroscopic binary star in the open cluster NGC 4755, which is also known as the Kappa Crucis Cluster or Jewel Box Cluster.
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This is a spectroscopic binary star system with a companion a mere 0.2 AU from the primary, assuming a distance of 71 parsecs, with an orbital period of 230 days.
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AG Draconis is a binary star system in the northern constellation of Draco. It consists of a giant star and a white dwarf that revolve around each other every 550 days.
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126 Tauri (126 Tau) is a blue subgiant star in the constellation Taurus. Its apparent magnitude is 4.83. It is also a binary star, with an orbital period of 111 years.
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Kepler-296 is a binary star system in the constellation Draco. The primary star appears to be a late K-type main-sequence star, while the secondary is a red dwarf.
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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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Artist's impression of the binary star system AR Scorpii The components of binary stars are denoted by the suffixes A and B appended to the system's designation, A denoting the primary and B the secondary. The suffix AB may be used to denote the pair (for example, the binary star α Centauri AB consists of the stars α Centauri A and α Centauri B.) Additional letters, such as C, D, etc., may be used for systems with more than two stars. In cases where the binary star has a Bayer designation and is widely separated, it is possible that the members of the pair will be designated with superscripts; an example is Zeta Reticuli, whose components are ζ1 Reticuli and ζ2 Reticuli.
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Lambda Crateris, Latinized from λ Crateris, is the Bayer designation for a suspected binary star system in the southern constellation of Crater. With an annual parallax shift of 23.32 milliarcsecond as observed from Earth, it is located around 140 light years from the Sun. It is faintly visible to the naked eye with an apparent visual magnitude of 5.08. This is a probable astrometric binary star system, with orbital elements first reported by Abt and Levy (1976).
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Pi5 Orionis (π5 Ori, π5 Orionis) is a binary star system in the constellation Orion. It has an apparent visual magnitude of 3.69, which is bright enough to be visible to the naked eye on a clear night. Based upon an annual parallax shift of 2.43 mas, it is around 1,300 light years distant from the Sun. This is a single-lined spectroscopic binary star system in a circular orbit with an orbital period of 3.7005 days.
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Phi Herculis (φ Her) is a binary star system in the northern constellation of Hercules. Based upon an annual parallax shift of 15.99 mas as seen from Earth, it is located around 204 light years from the Sun. With a combined apparent visual magnitude of 4.24, it is bright enough to be seen with the naked eye. This is a single-lined spectroscopic binary star system with an orbital period of 564.8 days and an eccentricity of 0.526.
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MY Camelopardalis (MY Cam) is a binary star system located in the Alicante 1 open cluster, some away in the constellation Camelopardalis. It is one of the most massive known binary star systems and a leading candidate for a massive star merger. MY Cam is the brightest star in Alicante 1. The system consists of two hot blue O-type stars with one component having a mass of 32 solar masses and the other 38 solar masses.
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The more massive member of the binary star 2MASS J1835, an M6.5 star, has strong X-ray activity indicative of a flare star, although it has never been directly observed to flare.
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Beta Lyrae type eclipsing binary star. Heavier, whiter component is surrounded with a gas ring. Gas comes to teardrop shaped secondary component. Beta Lyrae variables are a class of close binary stars.
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Gamma Leonis (γ Leonis, abbreviated Gamma Leo, γ Leo), also named Algieba , is a binary star system in the constellation of Leo. In 2009, a planetary companion around the primary was announced.
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Early in 1947, she went to live at the Abbey Art Centre, an artists' community located in New Barnet, Hertfordshire, near London.Eckett: "Binary Star", 7. King was a fairly early resident there.Gleeson, 25.
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KELT-4 is a triple star system. KELT-4BC is a binary star system subcomponent of the triple, away from KELT-4A and the projected separation between KELT-4B and KELT-4C is .
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HD 125040 is a visual binary star in the northern constellation Boötes. The pair orbit each other with a semi-major axis of 105 astronomical units and a period of roughly 750 years.
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An artist's rendering of the Epsilon Aurigae system. The most prominent variable star in Auriga is Epsilon Aurigae (Al Maz, Almaaz), an F0 class eclipsing binary star with an unusually long period of 27 years; its last minima occurred in 1982–1984 and 2009–2011. The distance to the system is disputed, variously cited as 4600 and 2,170 light-years. The primary is a white supergiant, and the secondary may be itself a binary star within a large dusty disk.
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Epsilon Librae (ε Lib) is the Bayer designation for a binary star system in the zodiac constellation Libra. With an apparent visual magnitude of 4.922, it is bright enough to be seen with the naked eye. Based upon an annual parallax shift of 32.02 mas, it is located about 102 light years away from the Sun. This is a single-lined spectroscopic binary star system. The pair orbit each other with a period of 226.9 days and an eccentricity of 0.66.
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Kepler-14 is a binary star system targeted by the Kepler spacecraft. It is host to one known planet: the Jupiter-like Kepler-14b. The star system was identified by Kepler as a possible planetary host, but when imaging revealed that Kepler-14 was a binary star system and not a single star, the confirmation process became protracted. The stars are separated by at least 280 AU, and the stars complete an orbit around a common center of mass every 2800 years.
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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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The star KELT-2A is a late F-dwarf and is one member of the common-proper-motion binary star system KELT-2. KELT-2B is an early K-dwarf about 295 AU away.
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It appears to be a binary star with a massive, possibly A-type secondary orbiting at a distance of around 1 astronomical unit. A fainter companion is separated from Theta Andromedae by 0.06 arcseconds.
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It is believed to be a binary star system. This star may be a member of the Scorpio- Centaurus OB association (Sco OB2). This is one of the nearest regions of recent star formation.
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The two constituents are designated δ¹ Tauri A and B. A is itself a binary star with components designated δ¹ Tauri Aa (officially named Secunda Hyadum , the traditional name for the entire system) and Ab.
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Delta Aquilae (δ Aquilae, δ Aql) is a binary star system in the equatorial constellation of Aquila. It has an apparent visual magnitude of 3.4 and, based upon parallax measurements, is located about from Earth.
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TOI 1338 is a binary star system located in the constellation Pictor, about 1,320 light-years from Earth. It was discovered by TESS and is orbited by a circumbinary planet known as TOI 1338 b.
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HD 74423 is a heartbeat binary star. HD 74423 A is said to be a sort of 'tear drop shape' and pulsates on only one side. This is caused by tidal interaction with its partner.
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HD 23089 is a spectroscopic binary star in the northern constellation of Camelopardalis. The system consists of a cooler giant star and hotter main sequence companion, with the pair orbiting each other every 6,150 days.
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Theta Circini (θ Cir), is a binary star located in the southern constellation of Circinus, to the northwest of Alpha Circini. It is faintly visible to the naked eye with an apparent visual magnitude of 5.110. Based upon an annual parallax shift of 11.82 mas, it is located at a distance of about 276 light years from the Sun. This is an astrometric binary star system with an orbital period of about 39.6 years, an eccentricity of 0.3, and a semimajor axis of 85.64 mas.
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HD 3322 is a binary star system in the northern constellation of Andromeda. With an apparent visual magnitude of 6.51, it lies below the nominal brightness limit for visibility with the normal naked eye, but it is still possible to see the star with excellent vision under ideal seeing conditions. An annual parallax shift of provides a distance estimate of roughly 700 light years. This is a single-lined spectroscopic binary star system with an orbital period of around 400 days and an eccentricity of 0.57.
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HD 214448 is a binary star system in the equatorial constellation of Aquarius. They orbit each other with a period of around 147 years. The combined mass of the pair is twice that of the Sun.
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The more massive gas giant is about 6 times the mass of Jupiter and orbits the binary star every 15.5 years, the other orbits every 7.75 years and is about 1.6 times the mass of Jupiter.
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This is the discography of the American hip-hop artist One Be Lo (aka OneManArmy). It also includes work with his groups Binary Star (with Senim Silla), Security (with Magestik Legend), and work from Subterraneous Records compilations.
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It is an orange-hued giant star of magnitude 2.5, 72 light-years from Earth. There are several other dimmer double and binary stars in Cygnus. Mu Cygni is a binary star with an optical tertiary component.
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This pair is at its greatest separation around 2019. Ten star systems have been found to have planets. Rho-1 Cancri or 55 Cancri (or Copernicus) is a binary star approximately 40.9 light-years distant from Earth.
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WZ Andromedae (abbreviated to WZ And) is an eclipsing binary star in the constellation Andromeda. Its maximum apparent visual magnitude is 11.6, but drops down to 12.00 during the main eclipse which occurs roughly every 16.7 hours.
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There is a remote chance that the Earth will instead be captured by a passing binary star system, allowing the planet's biosphere to remain intact. The odds of this happening are about one chance in three million.
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This is a double-lined spectroscopic binary star system. The spectrum matches a B-type main-sequence star with a stellar classification of B2.5 V. There is a faint visual companion with an apparent magnitude of 12.49.
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Kappa Cancri, Latinized from κ Cancri, is a blue-white hued binary star system in the zodiac constellation of Cancer. It is faintly visible to the naked eye with an apparent visual magnitude of +5.23. The magnitude difference between the two stars is about 2.6. Based upon an annual parallax shift of 7.13 mas as seen from the Earth, the system is located roughly 460 light years from the Sun. This is a single-lined spectroscopic binary star system with an orbital period of 6.39 days and an eccentricity of 0.13.
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Artist's impression of a low-mass X-ray binary (LMXB): an evolved low-mass yellow sub-giant star transfers mass to a neutron star. Because the accretor is a compact object, an accretion disc forms, which is the source of the X-rays. Source. An Interacting binary star is a type of binary star in which one or both of the component stars has filled or exceeded its Roche lobe. When this happens, material from one star (the donor star) will flow towards the other star (the accretor).
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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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Delta Scorpii (Latinised from δ Scorpii, abbreviated Delta Sco, δ Sco) is a binary star (the presence of a third star in the system is being debated) in the constellation of Scorpius. The primary star is named Dschubba .
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70 Ophiuchi is a binary star system located 16.6 light years away from the Earth. It is in the constellation Ophiuchus. At magnitude 4 it appears as a dim star visible to the unaided eye away from city lights.
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It regards females as unimportant. Alpha Centauri is also the name of Alpha Centauri's native star system. The Alpha Centauri binary star system is second only to Proxima Centauri in proximity to the Solar System, home to the Earth.
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Bayer-designated stars in Cassiopeia. Sigma Cassiopeiae is circled. Sigma Cassiopeiae (σ Cas, σ Cassiopeiae) is a binary star in the constellation Cassiopeia. It is approximately 5000 light years from Earth and has a combined apparent magnitude of +4.88.
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2MASS J19383260+4603591 (Also known as Kepler-451) is a binary star system with at least one known planet, Kepler-451b. The system comprises two stars, a subdwarf B-type star as well as a small red dwarf star.
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HD 169405, also known as HR 6894, is a suspected binary star system in the southern constellation of Telescopium, about a degree to the north of Zeta Telescopii. It is an orange K-type giant of spectral type K0.5III.
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XZ Andromedae (also known as XZ And) is a binary star in the constellation Andromeda. Its maximum apparent visual magnitude is 9.91, but drops down to 12.45 every 1.357 days. Its variability matches the behaviour of Algol variable stars.
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Gamma Virginis (γ Virginis, abbreviated Gamma Vir, γ Vir), officially named Porrima , is a binary star system in the constellation of Virgo. It consists of two almost identical main sequence stars at a distance of about 38 light years.
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They then plot the Spacer worlds on the ship's map, which form a rough sphere and conclude that the location of Earth must be near to the center of the sphere. This area turns out to have a binary star system.
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The General Catalogue of Variable Stars describes it as R:/PN, meaning it is likely a close binary star system with reflection of starlight being the cause of variation, as well as being part of the nucleus of a planetary nebula.
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Delta Virginis is a possible binary star, as an 11th magnitude star is located at an angular separation of 80 arcseconds. This K-type dwarf may have an orbital period of over 200,000 years, but this has not been confirmed.
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RV Corvi is an eclipsing binary star system in the constellation Corvus, ranging from apparent magnitude 8.6 to 9.16 over 18 hours. The system is composed of stars of spectral types F0 and G0, which orbit each other every 0.7473 days.
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HD 131473 is a binary star system in the northern constellation of Boötes. The primary is an F-type subgiant with a stellar classification of F4IV, while its companion is a G-type subgiant with a stellar classification of G1IV.
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HAT-P-4 is a wide binary star consisting of a pair of G-type main-sequence stars in the constellation of Boötes. It is also designated BD+36°2593. The star exhibits an infrared excess noise of unknown origin.
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Clarke was educated at the University of Oxford where she received a Doctor of Philosophy degree in 1987 for research on binary stars supervised by Geoffrey Bath. Her doctoral thesis was titled "Accretion disc structure in binary star and galactic potentials".
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R Canis Majoris is an eclipsing interacting binary star system in the constellation Canis Major. It varies from magnitude 5.7 to 6.34. The system is unusual in the low ratio between the main two components and shortness of the orbital period.
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AK Pictoris is a binary star. Its two stars orbit each other every 217.6 years, separated by 2.004″. The primary star is a G-type star with similar properties to the Sun. The secondary star is a K-type star.
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Astrophysics His research is primarily in the area of novae (thermonuclear explosions on white dwarf stars in binary star systems) and includes both theoretical work and observations using telescopes around the world and in space working across the electromagnetic spectrum.
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Binary star systems are common, found more frequently than single star systems like our own. The arrangement of HD 113766, a binary star system with a protoplanetary disk around one star, is somewhat similar to the one-half of the system HD 98800, which has been reported to have a large amount of warm dust mass at the equivalent distance of the solar system's asteroid belt. It is not currently known why both of these star systems should have such configurations; i.e. a protoplanetary disk around part of the system while other stars in the system lack one.
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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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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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They may also be detected by indirect techniques, such as spectroscopy (spectroscopic binaries) or astrometry (astrometric binaries). If a binary star happens to orbit in a plane along our line of sight, its components will eclipse and transit each other; these pairs are called eclipsing binaries, or, together with other binaries that change brightness as they orbit, photometric binaries. If components in binary star systems are close enough they can gravitationally distort their mutual outer stellar atmospheres. In some cases, these close binary systems can exchange mass, which may bring their evolution to stages that single stars cannot attain.
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36 Serpentis is a binary star system in the equatorial constellation of Serpens. It has the Bayer designation b Serpentis, while 36 Serpentis is the Flamsteed designation. The system is visible to the naked eye as a dim, white- hued point of light with a combined apparent visual magnitude of 5.09. It is located 162 light years away from the Sun based on parallax, and is moving closer with a radial velocity of −8 km/s. This is a spectroscopic binary star system with a long orbital period of 52.8 years and a high eccentricity of 0.83.
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Beta Trianguli (Beta Tri, β Trianguli, β Tri) is the Bayer designation for a binary star system in the constellation Triangulum, located about 127 light years from Earth. Although the apparent magnitude is only 3.0, it is the brightest star in the constellation Triangulum. This is a double-lined spectroscopic binary star system with an orbital period of 31.39 days and an eccentricity of 0.53. The members are separated by a distance of less than 5 AU. The primary component has a stellar classification of A5IV, indicating that it has evolved away from the main sequence and is now a subgiant star.
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Measurements of these variations can be used, for example, to determine the orbital period and the radii of the members of an eclipsing binary star system, the rotation period of a minor planet or a star, or the total energy output of supernovae.
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HD 88218 is a binary star in the southern constellation of Antlia. With an apparent magnitude of 6.16, the system is faintly visible to the naked eye from dark skies. The pair orbit each other with a period of about 86 years.
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Theta Aurigae (θ Aurigae, abbreviated Theta Aur, θ Aur) is a binary star in the constellation of Auriga. Based upon parallax measurements, the distance to this system is about . The two components are designated Theta Aurigae A (also named Mahasim) and B.
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Remember (stylized as R∃/MEMBER) is the third album by Hiroyuki Sawano's vocal project SawanoHiroyuki[nZk]. It was released on March 6, 2019, through the Sony Music label Sacra Music. Four singles were released from the album: "Binary Star", "Cage", "narrative" and "NOISEofRAIN".
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WASP-11/HAT-P-10 is a binary star. It is a primary main-sequence orange dwarf star. Secondary is M-dwarf with a projected separation of 42 AU. The system is located about 408 light years away in the constellation Aries.
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Cygnus X was a trance music project from Germany named after the famous X-ray binary star Cygnus X-1. It began as a collaboration between Matthias Hoffmann and Ralf Hildenbeutel, who later left.Cygnus X profile. Discogs. Retrieved on 17 January 2008.
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WR 25 (HD 93162) is a binary star system in the turbulent star forming region Carina Nebula, about 6,800 light-years from Earth. It contains a Wolf-Rayet star and a hot luminous companion, and is a member of the Trumpler 16 cluster.
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Alpha Trianguli (α Trianguli, abbreviated Alpha Tri, α Tri) is a spectroscopic binary star in the constellation of Triangulum. Based on parallax measurements obtained during the Hipparcos mission, it is approximately distant from the Sun. The brighter or primary component is named Mothallah .
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It has about the same mass as the Sun, but has expanded to 44.7 times the Sun's radius. The star is radiating 391 times the solar luminosity. It is 366 ± 8 light-years distant from the Sun. Zeta Crateris is a binary star system.
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The competing scenario, that the system was formed out of a binary star system consisting of two normal (main sequence) stars, is not ruled out but is disfavored as black holes formed in such a binary are more likely to have positively aligned spins.
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A planet orbiting one of the stars was discovered through astrometric observations. However, it is not known which stellar component the planet is orbiting around. The parent star is a binary star. The planet parameters are given for the component B (Muterspaugh et al. 2010).
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CD Crucis, also known as HD 311884, is an eclipsing binary star system in the constellation Crux. It is around 14,000 light years away near the faint open cluster Hogg 15. The binary contains a Wolf–Rayet star and is also known as WR 47.
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HD 205877 is a visual binary star system in the constellation Indus. It also a double lined spectroscopic binary. The components are very similar and both are located on the giant branch in the Hertzsprung–Russell diagram in agreement with the F7III spectral type.
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HD 156411 is a star hotter and larger than the sun with a gas giant planet in orbit. Gliese 674 is a nearby red dwarf star with a planet. Gliese 676 is a binary star system composed of two red dwarves with four planets.
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This binary star was found variable by Henrietta Leavitt, and shows the usual two eclipses, a main one and a secondary one with a less pronounced drop in magnitude. The period of 16.7 days, however, was found to vary in time without any consolidated trend.
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The primary component, Atlas A, is a blue-white B-type giant with an apparent magnitude of +3.62. It is a binary star whose components have magnitudes of 3.84 and 5.46. The binary makes one orbit every 290 days, and the eccentricity is about 0.24.
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Astrosat-1 in deployed configuration Astrosat is India's first multi wavelength space observatory and full-fledged astronomy satellite. Its observation study includes active galactic nuclei, hot white dwarfs, pulsations of pulsars, binary star systems, supermassive black holes located at the centre of the galaxies, etc.
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Beta Crateris, Latinized from β Crateris, is a binary star system in the southern constellation of Crater. It is visible to the naked eye with an apparent visual magnitude of 4.46. Based upon an annual parallax shift of 9.59 mas as seen from Earth, it is located around 340 light years from the Sun. This is an astrometric binary star system with an orbital period of 6.0 years and a projected separation of 8.3 AU. The orbit has an estimated semimajor axis of 9.3 AU. The primary, component A, is listed as an A-type giant star with a stellar classification of A2 III.
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The very active star-forming region around the Tarantula Nebula in the Large Magellanic Cloud, where VFTS 352 is located VFTS 352 is a contact binary star system away in the Tarantula Nebula, which is part of the Large Magellanic Cloud. It is the most massive and earliest spectral type overcontact system known. The discovery of this O-type binary star system made use of the European Southern Observatory's Very Large Telescope, and the description was published on 13 October 2015. VFTS 352 is composed of two very hot (40,000 °C), bright and massive stars of equal size that orbit each other in little more than a day.
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Chi2 Hydrae, Latinised from χ2 Hydrae, is a binary star system in the equatorial constellation of Hydra. Based upon an annual parallax shift of 4.6 mas as seen from Earth, it is located roughly 710 light years from the Sun. It is visible to the naked eye with a combined apparent visual magnitude of 5.71. This is a detached eclipsing binary star system with an orbital period of 2.27 days and an essentially circular orbit having a measured eccentricity of 0.00. The eclipse of the primary by the secondary component reduces the visual magnitude of the system by 0.29, while the eclipse of the secondary diminishes the magnitude by 0.27.
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The star system, Kepler-1647 (also known as 2MASS J19523602+4039222, KOI-2939, and KIC 5473556), is a binary star with the primary star (Kepler-1647 A) having a mass of 1.22 , a radius of 1.79 , and a surface temperature of 6210 ± 100 K. The secondary star (Kepler-1647 B), on the other hand, has a mass of 0.975 , a radius of 1.79 , and a surface temperature of 5770 K. In comparison, the Sun has a surface temperature of 5778 K. The two orbit each other every 11 days. The binary star system's age is estimated to be about 4.4 billion years old, about 200 million years younger than the Sun.
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Xi Boötis (ξ Boo, ξ Boötis) is a binary star system 22 light years away from Earth. It is the nearest visible star in the constellation Boötes. The brighter, primary component of the pair has a visual magnitude of 4.70, making it visible to the naked eye.
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A hypothetical rendition of the Blue Moon orbiting high above the plane of its parent gas giant planet. The second episode of the program focuses on a fictional moon called the Blue Moon, which orbits an enormous gas giant that is itself orbiting a binary star system.
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The projected separation of the two components is , or . Proper motion measurements for the two stars are almost identical making HD 91324 a likely binary star system. The photometry of 2MASS J10313234–5338010 is consistent with it being a red dwarf of spectral type M5 or M6.
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V923 Aquilae is a Be star in the equatorial constellation of Aquila. It is a binary star with a low mass secondary star orbiting at a separation of around 250 times the radius of the Sun. The primary varies with both short term and long term periodicity.
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26 Aurigae is a binary star system in the northern constellation of Auriga. It is visible to the naked eye as a faint star with an apparent visual magnitude of 5.41. The distance to this system remains poorly constrained. The new Hipparcos reduction gives a parallax of .
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It is unusual because of its strong silicon emission lines. The constellation is home to several double stars, including Epsilon, Lambda, and Pi Arietis. ε Arietis is a binary star with two white components. The primary is of magnitude 5.2 and the secondary is of magnitude 5.5.
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CN Andromedae (CN And) is an eclipsing binary star in the constellation Andromeda. Its maximum apparent visual magnitude is 9.62 and drops down to a minimum of 10.2 during the main eclipse. It's classified as a Beta Lyrae variable with a period roughly of 0.4628 days.
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EE Pegasi is an eclipsing binary star system in the constellation Pegasus. The two main components are two main sequence stars of spectral types A3V and F5V, with a third, smaller, star that is an orange or red dwarf orbiting the main pair every four years.
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In close binary star systems one of the stars can lose mass to a heavier companion. Accretion- powered pulsars may drive mass loss. The shrinking star can then become a planetary-mass object. An example is a Jupiter-mass object orbiting the pulsar PSR J1719-1438.
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The secondary is of magnitude 6. κ Gem is a binary star 143 light-years from Earth. The primary is a yellow giant of magnitude 3.6; the secondary is of magnitude 8. The two are only divisible in larger amateur instruments because of the discrepancy in brightness.
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Kappa Scorpii, Latinized from κ Scorpii, is a binary star system in the southern constellation of Scorpius. With an apparent visual magnitude of 2.4, this star system is readily visible to the naked eye. Parallax measurements place it at an estimated distance of roughly from the Earth.
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M Centauri (M Cen) is a binary star in the constellation Centaurus. It is approximately 260 light years from Earth. M Centauri is a yellow G-type giant with an apparent magnitude of +4.64. It is a spectroscopic binary with an orbital period of 437 days.
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HD 42936 is a binary star composed of an orange (K-type) main-sequence star and an L-type dwarf star just massive enough to burn hydrogen, located approximately 153 light-years away in the constellation of Mensa, taking its primary name from its Henry Draper Catalogue designation.
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Beta Delphini (β Delphini, abbreviated Beta Del, β Del) is a binary star in the constellation of Delphinus. It is the brightest star in Delphinus. The two components of the system are designated Beta Delphini A (officially named Rotanev , which is historically the name of the system) and B.
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Collisions occur with greater frequency in the dense core regions of globular clusters (cf. blue stragglers). A likely scenario is a collision with a binary star system, or between two binary systems containing white dwarfs. This collision can leave behind a close binary system of two white dwarfs.
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HD 180555 is a binary star in the equatorial constellation of Aquila. It consists of a two stars, orbiting with an orbital period of 8.95 years and an eccentricity of 0.43. A third component lies at an angular separation of 8.32″, but it is unrelated to the system.
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AB7, also known as SMC WR7, is a binary star in the Small Magellanic Cloud. A Wolf–Rayet star and a supergiant companion of spectral type O orbit in a period of 19.56 days. The system is surrounded by a ring-shaped nebula known as a bubble nebula.
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Sculpture "Binary star" at Kopal's birthplace in Litomyšl. It was made of kevlar fibers by Federico Díaz and Marian Karel. Zdeněk Kopal (; 4 April 1914 - 23 June 1993) was a Czech astronomer who mainly worked in England. Kopal was born and grew up in Litomyšl (Czechoslovakia, now Czech Republic).
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HD 32450, also known as Gliese 185 is a binary star in the constellation Lepus. It is located about 28 light years from the Solar System. This star will make its closest approach to the Sun in roughly 350,000 years, when it comes within . See Table 4, p. 644.
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TW Andromedae (TW And) is an eclipsing binary star, classified also as an Algol variable star, in the constellation Andromeda. Its brightness varies with a period of 4.12 days, and has a typical brightness of magnitude 8.98 but decreasing down to a magnitude of 11.04 during the main eclipse.
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Edward M Sion (born January 18, 1946) is an American astrophysicist who is Professor in the Department of Astrophysics and Planetary Science at Villanova University. He specializes on the structure and evolution of white dwarf stars and white dwarf stars in explosive binary star systems known as cataclysmic variables.
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DS Andromedae (often abbreviated to DS And) is an eclipsing binary star in the constellation Andromeda and a member of the open cluster NGC 752. Its maximum apparent visual magnitude is 10.44, but drops down to 10.93 during the main eclipse and to 10.71 during the secondary one.
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One of the nearest known black holes to our Solar System is in this constellation. The binary star system A0620-00 in the constellation of Monoceros is at a distance of about roughly 3,300 light- years (1,000 parsecs) away. The black hole is estimated to be 6.6 solar masses.
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VB 10 or Van Biesbroeck's star Charles Earle Funk (1936) What's the Name, Please?: A Guide to the Correct Pronunciation of Current Prominent Names, p.161 is a very small and very dim red dwarf located in the constellation Aquila. It is part of a binary star system.
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Alpha Coronae Borealis (α Coronae Borealis, abbreviated Alpha CrB, α CrB), officially named Alphecca , is an eclipsing binary star in the constellation of Corona Borealis. It is located about 75 light years from the Sun and contains two main sequence stars, one class A and one class G.
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Recent studies derive a distance around 1,250 pc for the M8 region. Erosion of the front of the molecular cloud apparently caused by 9 Sgr suggests that it lies in front of the cloud, but studies of 9 Sgr as a binary star give a distance of 1,790 pc.
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Phi2 Cancri (φ2 Cancri) is a binary star in the constellation Cancer, about 280 light-years from Earth. Both components are white A-type main sequence dwarfs with apparent magnitudes of +6.3. They are separated by 5.126 arcseconds on the sky, and their mean apparent brightness is +5.55 magnitudes.
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The magnitude 5.97 secondary, component B, is a single-lined spectroscopic binary star system with an orbital period of 17.4 days and an eccentricity of 0.21. The pair have an angular separation of . The visible component is a B-type main-sequence star with a class of B8 V.
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The planet orbits in a circumbinary (M-type) binary star system named OGLE-2007-BLG-349L. They orbit around each other roughly every 9 days. The stars have masses of 0.41 and 0.30 , respectively. The age of the system, radii and temperatures of the stars are not known.
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It is not uncommon that the accretion disc is the brightest (and thus sometimes the only visible) element of a binary star. If a star grows outside of its Roche lobe too fast for all abundant matter to be transferred to the other component, it is also possible that matter will leave the system through other Lagrange points or as stellar wind, thus being effectively lost to both components."Mass Transfer in Binary Star Systems" by Jeff Bryant with Waylena McCully, Wolfram Demonstrations Project. Since the evolution of a star is determined by its mass, the process influences the evolution of both companions, and creates stages that cannot be attained by single stars.
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Another warned her that he had received his mobilisation papers and that she should leave as soon as possible. She spent about a year in domestic service with families in southern England.Eckett, "Binary Star", 5. She found England far more old-fashioned and conservative than the Berlin she had come from.
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Sky over Paranal. γ Volantis is in the centre of the image, above (actually northeast of) the Large Magellanic Cloud. Gamma Volantis, Latinized from γ Volantis, is a wide binary star system in the southern constellation of Volans. Based upon parallax measurements, it is approximately 142 light years from Earth.
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Upsilon Sagittarii (Upsilon Sgr, υ Sagittarii, υ Sgr) is a spectroscopic binary star system in the constellation Sagittarius. Upsilon Sagittarii is the prototypical hydrogen-deficient binary (HdB), and one of only four such systems known. The unusual spectrum of hydrogen-deficient binaries has made stellar classification of Upsilon Sagittarii difficult.
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This star is one of the brightest known extreme ultraviolet sources in the sky. It is a binary star; the secondary is of magnitude 7.4. Its traditional name means "the virgins", having been transferred from the group of stars to Epsilon alone. Nearby is Delta Canis Majoris, also called Wezen.
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Other notable objects in Caelum are RR Caeli, a binary star with one known planet approximately away; X Caeli, a Delta Scuti variable that forms an optical double with γ 1 Caeli; and HE0450-2958, a Seyfert galaxy that at first appeared as just a jet, with no host galaxy visible.
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HD 114762 is a binary star system approximately away in the constellation Coma Berenices. It consists of a yellow-white F-type main-sequence star and a red or brown dwarf companion approximately distant. Both are low-metal subdwarfs. A telescope or strong binoculars are needed to view the primary.
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40 Arietis is a probable binary star system in the northern constellation of Aries. 40 Arietis is the Flamsteed designation. Their combined apparent magnitude is 5.82, putting the system near the limit of naked eye visibility. Based upon an annual parallax shift of just , it is away from the Sun.
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QR Andromedae (often abbreviated to QR And) is an eclipsing binary star in the constellation Andromeda. Its maximum apparent visual magnitude is 12.16, but its light curve shows clearly eclipsing events where its brightness can drop to a magnitude of 13.07. This leads to its classification as an Algol variable star.
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There are 305 candidate members with a probability of 95% or higher, and up to 4,349 with a 50% membership probability. The cluster metallicity is given by [Fe/H] = . Of 418 probable cluster members, Leiner et al. (2015) found 64 that have variable radial velocities and thus are binary star systems.
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Epsilon Sagittarii (Latinised from ε Sagittarii, abbreviated Epsilon Sgr, ε Sgr), formally named Kaus Australis , is a binary star system in the southern zodiac constellation of Sagittarius. The apparent visual magnitude of +1.85 makes it the brightest object in Sagittarius. Based upon parallax measurements, this star is around from the Sun.
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Cor Caroli seen from northern England on March 1, 2011. Alpha Canum Venaticorum is a binary star with a combined apparent magnitude of 2.81. The two stars are 19.6 arcseconds apart in the sky and are easily resolved in small telescopes. The system lies approximately 110 light years from the Sun.
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88 Tauri B, 69.56 arcseconds away, is a seventh-magnitude star that is also a binary star system. It is another spectroscopic binary whose components (88 Tauri Ba and Bb) orbit each other every 3.69 years. The orbit of 88 Tauri B around 88 Tauri A likely takes about 70,000 years.
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Upsilon Aquarii (υ Aqr, υ Aquarii) is the Bayer designation for a binary star in the equatorial constellation of Aquarius. It is a faint naked eye star with an apparent visual magnitude of 5.21. Parallax measurements give a distance estimate of from Earth. This is a high proper-motion star.
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Kepler-34 is an eclipsing binary star system in the constellation of Cygnus. Both stars have roughly the same mass as the Sun, therefore both are spectral class G. They are separated by 0.22 AU, and complete an eccentric (e=0.5) orbit around a common center of mass every 27 days.
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Paula Szkody specializes in cataclysmic variable stars, which are binary star systems that periodically undergo energetic outbursts. She is an active participant in the Sloan Digital Sky Survey (SDSS) searching for new dwarf novae and has worked with the XTE, ASCA, ROSAT, IUE, HST, EUVE and XMM-Newton space missions.
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In 2017 KIC 9832227, a binary star system, was predicted to merge and produce a red nova by early 2022. In September 2018, a typo was discovered in data used for the initial prediction, and it was determined that the merger would likely not take place at the predicted time.
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VB 10 is the secondary star of a bound binary star system. The primary is called Gliese 752, and hence VB 10 is also referred to as Gliese 752 B. The primary star is much larger and brighter. The two stars are separated by about 74 arc seconds (~434 AU).
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WR 142 is a Wolf-Rayet star in the constellation Cygnus, an extremely rare star on the WO oxygen sequence. It is a luminous and very hot star, highly evolved and close to exploding as a supernova. It is suspected to be a binary star with a companion orbiting about away.
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Epsilon Boötis (ε Boötis, abbreviated Epsilon Boo, ε Boo), officially named Izar , is a binary star in the northern constellation of Boötes. The star system can be viewed with the unaided eye at night, but resolving the pair with a small telescope is challenging; an aperture of or greater is required.
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BD Camelopardalis is an S star and symbiotic star in the constellation Camelopardalis. It was recognized as a spectroscopic binary star in 1922, and its orbital solution published in 1984; it has a 596-day orbital period. A spectroscopic composition analysis was done of the red giant primary star in 1986.
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Waterworld is the debut album from Michigan hip hop duo Binary Star. The album was self-released, with only 1,000 copies printed. A rearranged, remixed version was created the following year, Masters of the Universe, with wider distribution. The entire album was recorded, mixed and mastered on a $500 budget.
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WOH G64 has a possible late O-type dwarf companion of a bolometric magnitude of −7.5 or a luminosity of , which would make WOH G64 a binary star although there has been no confirmation of this observation and the intervening dust clouds makes the study of the star very difficult.
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The MgI line: a new probe of the atmospheres of evaporating exoplanets The water vapour was detected in planetary atmosphere in 2018. The star KELT-2A is a member of the common- proper-motion binary star system KELT-2 (HD 42176). KELT-2B is an early K dwarf approximately 295 astronomical units away.
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There is a nearby companion star of class A0 IV located at an angular separation of 0.1 arc seconds along a position angle of 179°, as of 2002. Schöller et al. (2010) consider this to be a visual companion, although Eggleton and Tokovinin (2008) listed the pair as a probable binary star system.
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V Puppis (V Pup) is a star system in the constellation Puppis. Its apparent magnitude is 4.41. There is a binary star system at the center with a B1 dwarf orbiting a B3 subgiant star. They have an orbital period of 1.45 days and a distance of only 15 solar radii apart.
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HD 21447 is a probable binary star system located in the constellation Camelopardalis. The star is also known as HR 1046. It can be viewed with the naked eye, having an apparent visual magnitude of 5.09. Based upon an annual parallax shift of , it is located some 199 light years from the Sun.
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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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35 Arietis (abbreviated 35 Ari) is a binary star in the northern constellation of Aries. 35 Arietis is the Flamsteed designation. It is approximately distant from the Earth, based upon an annual parallax shift of 9.51 mas. This star is visible to the naked eye with an apparent visual magnitude of 4.64.
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33 Arietis (abbreviated 33 Ari) is a binary star in the northern constellation of Aries. 33 Arietis is the Flamsteed designation. The combined apparent magnitude of 5.33 is bright enough to be seen with the naked eye. Based upon an annual parallax shift of 14.09 mas, the distance to this system is approximately .
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Tau Boötis, Latinized from τ Boötis, is an F-type main-sequence star approximately 51 light-years away in the constellation of Boötes. It is a binary star system, with the secondary star being a red dwarf. As of 1999, an extrasolar planet has been confirmed to be orbiting the primary star.
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With his illusions dispersed, Sadow's forces were forced to retreat. Upon returning to Sith space, they found that Kressh had not been killed, and engaged him in a space battle. Sadow was victorious again, but they were soon attacked by Republic forces. Sadow escaped by causing the Denarii Binary Star to go supernova.
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The Cor Caroli system is a binary star designated Alpha Canum Venaticorum (α Canum Venaticorum, abbreviated Alpha CVn, α CVn). The International Astronomical Union uses the name "Cor Caroli" specifically for the brighter star of the binary. Alpha Canum Venaticorum is the brightest point of light in the northern constellation of Canes Venatici.
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One of his publications was on the study of the binary star system Beta Lyrae, which was published in the American Philosophical Society. The publication provided solutions to old problems about the systems of closed binary stars. Later astronomer Helmut Abt in the United States would confirm that the work was correct.
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Antares appears as a single star when viewed with the naked eye, but it is actually a binary star, with its two components called α Scorpii A and α Scorpii B. The brighter of the pair is the red supergiant, while the fainter is a hot main sequence star of magnitude 5.5.
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Eta Pegasi (η Pegasi, abbreviated Eta Peg, η Peg), formally named Matar , is a binary star in the constellation of Pegasus. The apparent visual magnitude of this star is +2.95, making it the fifth-brightest member of Pegasus. Based upon parallax measurements, the distance to this star is about from the Sun.
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It is radiating 89 times the luminosity of the Sun from its enlarged photosphere at an effective temperature of 4,400 K. Kappa Leonis has a magnitude 10.4 companion at an angular separation of 2.1 arc seconds. The pair most likely form a binary star system. The companion is a suspected variable star.
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10 Ursae Majoris is a binary star system in the northern constellation of Lynx. It is visible to the naked eye as a faint star with a combined apparent visual magnitude of 3.960. This system is fairly close to the Sun, at away from Earth. It is the third-brightest object in Lynx.
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Alpha Piscium (α Piscium) is a binary star system in the equatorial constellation of Pisces. Based upon parallax measurements made by the Hipparcos spacecraft, it is located approximately 311 light-years from the Sun. The two components are designated Alpha Piscium A (officially named Alrescha, the traditional name of the system) and B.
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Luyten 726-8, also known as Gliese 65, is a binary star system that is one of Earth's nearest neighbors, at about 8.7 light years from Earth in the constellation Cetus. Luyten 726-8B is also known under the variable star designation UV Ceti, being the archetype for the class of flare stars.
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Hydra has one bright binary star, Epsilon Hydrae, which is difficult to split in amateur telescopes; it has a period of 1000 years and is 135 light-years from Earth. The primary is a yellow star of magnitude 3.4 and the secondary is a blue star of magnitude 6.7. However, there are several dimmer double stars and binary stars in Hydra. 27 Hydrae is a triple star with two components visible in binoculars and three visible in small amateur telescopes. The primary is a white star of magnitude 4.8, 244 light-years from Earth. The secondary, a binary star, appears in binoculars at magnitude 7.0 but is composed of a magnitude 7 and a magnitude 11 star; it is 202 light-years from Earth. 54 Hydrae is a binary star 99 light-years from Earth, easily divisible in small amateur telescopes. The primary is a yellow star of magnitude 5.3 and the secondary is a purple star of magnitude 7.4. N Hydrae (N Hya) is a pair of stars of magnitudes 5.8 and 5.9. Struve 1270 (Σ1270) consists of a pair of stars, magnitudes 6.4 and 7.4.
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The Palomar Observatory confirmed findings suggesting that Kepler-14 was a binary star. The Fibre-fed Échelle Spectrograph (FIES) on the Canary Islands' Nordic Optical Telescope was operated in October 2009, using Doppler spectroscopy to gather information that would accompany the gathered photometric observations. The High Resolution Échelle Spectrometer (HIRES) at the W.M. Keck Observatory was also utilized. Use of the WIYN Observatory for speckle imaging found that the host star of KOI-98 was actually a close-knit binary star, which complicated the analysis. A November 2009 operation of the ARIES instrument on the MMT Observatory and the July 2010 use of the PHARO near-infrared camera on the Palomar Observatory's 200 inch Hale telescope used adaptive optics to confirm WIYN's findings.
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The masses of the two pre-merger black holes provide information about stellar evolution. Both black holes were more massive than previously discovered stellar-mass black holes, which were inferred from X-ray binary observations. This implies that the stellar winds from their progenitor stars must have been relatively weak, and therefore that the metallicity (mass fraction of chemical elements heavier than hydrogen and helium) must have been less than about half the solar value. The fact that the pre-merger black holes were present in a binary star system, as well as the fact that the system was compact enough to merge within the age of the universe, constrains either binary star evolution or dynamical formation scenarios, depending on how the black hole binary was formed.
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Artist's impression of a young binary star system at periastron Pulsed Accretion in astronomy is the periodic modulation in accretion rate of young stellar objects in binary systems, producing a periodic pulse in the observed infrared light curves of T Tauri stars. In double stars in young stellar objects, a protoplanetary disk is formed around each star, accreted from matter close to the star. In such a binary star system a strongly eccentric orbit produces strong gravitational forces on the circumstellar disks at periastron, and such disturbance can lead to a temporary increase in the accretion rate onto the star. This increased accretion rate leads to a change of intensity in the infrared, such intensity rising by up to tenfold in the protostar LRLL 54361.
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By 1803, he had observed changes in the relative positions in a number of double stars over the course of 25 years, and concluded that they must be binary systems; the first orbit of a binary star, however, was not computed until 1827, when Félix Savary computed the orbit of Xi Ursae Majoris.p. 291, French astronomers, visual double stars and the double stars working group of the Société Astronomique de France, E. Soulié, The Third Pacific Rim Conference on Recent Development of Binary Star Research, proceedings of a conference sponsored by Chiang Mai University, Thai Astronomical Society and the University of Nebraska-Lincoln held in Chiang Mai, Thailand, 26 October-1 November 1995, ASP Conference Series 130 (1997), ed. Kam-Ching Leung, pp. 291–294, .
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This distortion occurs because the star is spinning extremely rapidly. There are several other noteworthy stars in Eridanus, including some double stars. Beta Eridani, traditionally called Cursa, is a blue-white star of magnitude 2.8, 89 light- years from Earth. Its place to the south of Orion's foot gives it its name, which means "the footstool". Theta Eridani, called Acamar, is a binary star with blue-white components, distinguishable in small amateur telescopes and 161 light-years from Earth. The primary is of magnitude 3.2 and the secondary is of magnitude 4.3. 32 Eridani is a binary star 290 light-years from Earth. The primary is a yellow-hued star of magnitude 4.8 and the secondary is a blue-green star of magnitude 6.1.
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In astronomy, the distance to a visual binary star may be estimated from the masses of its two components, the size of their orbit, and the period of their orbit about one another. A dynamical parallax is an (annual) parallax which is computed from such an estimated distance. To calculate a dynamical parallax, the angular semi-major axis of the orbit of the stars is observed, as is their apparent brightness. By using Newton's generalisation of Kepler's Third Law, which states that the total mass of a binary system multiplied by the square of its orbital period is proportional to the cube of its semi-major axis, together with the mass-luminosity relation, the distance to the binary star can then be determined.
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Despite its youth, it shows an enhancement of Alpha process elements. Possibly this is due to an enhancement of its birth molecular cloud by a nearby Type II supernova explosion. At least nine variable star members have been identified with high probability, plus 29 lower probability members. The former include two eclipsing binary star systems.
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Further observations suggested a possible rotation period of around 42 days. Samus et al. (2017) classify it as a suspected RS Canum Venaticorum variable, meaning that it is a close binary star whose components have star-spots that cause rotationally-modulated variations in brightness. It has been given the variable star designation V2008 Cygni.
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HD 64440, also known as a Puppis, is a spectroscopic binary star in the constellation Puppis. Its apparent magnitude is 3.71. Located around distant, the primary is a bright giant of spectral type K1.5II and the secondary is an early A-type star. They orbit with a period just under 7 years and eccentricity 0.38.
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AM Canum Venaticorum (AM CVn) is a hydrogen-deficient cataclysmic variable binary star in the constellation of Canes Venatici. It is the type star of its class of variables, the AM Canum Venaticorum stars. The system consists of a white dwarf gaining matter via an accretion disk from a semi-degenerate or white dwarf companion.
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Iota Cassiopeiae is known to be a quintuple star system. The brightest star system, ι Cassiopeiae A, contains a white-colored A-type main-sequence star with a mean apparent magnitude of +4.61. The primary component is a tighter binary star system itself. The two stars themselves were resolved by adaptive optics, revealing two stars.
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According to Eggleton and Tokovinin (2008), this is a suspected binary star system with an orbital period of 4.9 days and an eccentricity of 0.2. However, De Rosa et al. (2014) did not find a companion. The primary is metallic-lined (Am) star, meaning it has unusually strong absorption lines of metals in its spectrum.
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9 Cygni is a binary star system in the northern constellation of Cygnus. 9 Cygni is its Flamsteed designation. The two stars have a combined magnitude of 5.39, so it can be seen with the naked eye under good viewing conditions. Parallax measurements made by Gaia put the star at a distance of around () away.
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4U 0614+091 is a low-mass X-ray binary star system which features a neutron star and a low-mass companion star. The binary system lies 10,000 light-years away in Orion. It produces jets like a microquasar, the first time an object other than a black hole has been shown to produce jets.
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Zeta1 Lyrae, Latinized from ζ1 Lyrae, is a binary star in the northern constellation of Lyra. Based upon an annual parallax shift of 20.89 mas as seen from Earth, the pair are located about 156 light years from the Sun. It is visible to the naked eye with an apparent visual magnitude of 4.37.
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HD 73390, also called e1 Carinae, is a binary star system in the constellation Carina. It is approximately 870 light years from Earth. The primary is a blue- white B-type main sequence dwarf with an apparent magnitude of +5.27. It displays an infrared excess and is a candidate host of an orbiting debris disk.
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This is a spectroscopic binary star system with an estimated period of 2,500 days. The primary component is a red giant star with a stellar classification of M1.5 III. The outer envelope of this evolved star has expanded to 35 times the size of the Sun. The star has the same mass as the Sun.
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Nahshid Sulaiman (born Ralond Scruggs; November 7, 1976), better known by his stage name One Be Lo, is an alternative hip hop artist from Pontiac, Michigan. He is well respected for being one half of the rap duo Binary Star, and has released a number of well-received solo albums.SoundSlam.com 2008 One.Be.Lo: R.E.B.I.R.T.H. Retrieved Jan.
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Some Wolf–Rayet stars are surrounded by pinwheel nebulae. These nebulae are formed from the dust that is spewed out of a binary star system. The stellar winds of the two stars collide and form two dust lanes that spiral outward with the rotation of the system. An example of this is WR 104.
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Chini et al. (2012) identify this as a double-lined spectroscopic binary star system. It shows a stellar classification of O9.7 Iab, matching a massive O-type supergiant star. Along with the O-type star 16 Sgr (HD 167263), it is ionizing an H II region along the western edge of the molecular cloud L291.
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BG Geminorum is an eclipsing binary star system in the constellation Gemini. It consists of a K0 supergiant with a more massive but unseen companion. The companion is likely to be either a black hole or class B star. Material from the K0 star is being transferred to an accretion disk surrounding the unidentified object.
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Tau1 Eridani, Latinized from τ1 Eridani, is a binary star system in the constellation Eridanus. It has an apparent magnitude of 4.46, making it visible to the naked eye in suitably dark conditions. This a spectroscopic binary with an orbital period of 958 days. It is located about 46 light years from the Earth.
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Gliese 777, often abbreviated as Gl 777 or GJ 777, is a yellow subgiant approximately 52 light-years away in the constellation of Cygnus. The system is also a binary star system made up of two stars and possibly a third. As of 2005, two extrasolar planets are known to orbit the primary star.
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Tau5 Eridani, Latinized from τ5 Eridani, is a binary star system in the constellation Eridanus. It is visible to the naked eye with a combined apparent visual magnitude of 4.26. The distance to this system, as estimated using the parallax technique, is around 293 light years. Tau5 Eridani is a double-lined spectroscopic binary system.
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Kepler-432 is a binary star system composed of a K-type giant star (Kepler-432 A) and a red dwarf star (Kepler-432 B). The apparent magnitude of the system, or how bright it appears from Earth's perspective, is about 15.8. Therefore, it is too dim to be seen with the naked eye.
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Delta Equulei, Latinized from δ Equulei, is the second brightest star in the constellation Equuleus. Delta Equulei is a binary star system about 60 light years away, with components of class G0 and F5. Their combined magnitude is 4.47, and their absolute magnitude is 3.142. There is controversy as to the exact masses of the stars.
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Pi Virginis (π Vir, π Virginis) is a binary star in the zodiac constellation of Virgo. It is visible to the naked eye with an apparent visual magnitude of 4.64. The distance to this star, based upon parallax measurements, is roughly 380 light years. This is a spectroscopic binary system with a stellar classification of A5V.
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Beta Aquilae (β Aquilae, abbreviated Beta Aql, β Aql) is a binary star in the equatorial constellation of Aquila. Based on parallax measurements obtained during the Hipparcos mission, it is approximately 44.7 light-years from the Sun. Its two components are designated Beta Aquilae A (formally named Alshain , the traditional name for the system) and B.
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Mimosa , designated β Crucis (Latinised to Beta Crucis, abbreviated Beta Cru, β Cru), is the second-brightest object in the constellation of Crux, after Acrux (Alpha Crucis), and the 20th-brightest star in the night sky. It forms part of the prominent asterism called the Southern Cross. Mimosa is a binary star or a possible triple star system.
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WR 22, also known as V429 Carinae or HR 4188, is an eclipsing binary star system in the constellation Carina. The system contains a Wolf-Rayet (WR) star that is one of the most massive and most luminous stars known, and is also a bright x-ray source due to colliding winds with a less massive O class companion.
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KOI-74 () is an eclipsing binary star in the constellation of Cygnus. The primary star is an A-type main-sequence star with a temperature of . It lies in the field of view of the Kepler Mission and was determined to have a companion object in orbit around it which is smaller and hotter than the main star.
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27 Piscium is a binary star system in the zodiac constellation of Pisces. It is visible to the naked eye with an apparent visual magnitude of 4.88. Based upon an annual parallax shift of , it is located about 234 light years away. The system is positioned near the ecliptic and so is subject to occultation by the Moon.
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U Coronae Borealis (U CrB) is an Algol-type eclipsing binary star system in the constellation Corona Borealis. Its apparent magnitude varies between 7.66 and 8.79 over a period of 3.45 days The component stars are a blue-white main sequence star of spectral type B6V and a cooler yellow-white subgiant star of spectral type F8III-IV.
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Funspot has a working arcade machine in an all-yellow cabinet. An original arcade version of Death Race is present in the Musée Mécanique in San Francisco. The Galloping Ghost Arcade in Brookfield, Illinois, received an original black cabinet as a donation. In 2016 Binary Star Software released a dual title cartridge called "Nox / Death Chase".
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Located near Eta Cygni is the X-ray source Cygnus X-1, which is now thought to be caused by a black hole accreting matter in a binary star system. This was the first x-ray source widely believed to be a black hole. The two component stars of Albireo are easily distinguished, even in a small telescope.
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30 Persei is a binary star system in the northern constellation Perseus. It is faintly visible to the naked eye with an apparent visual magnitude of 5.49. Based upon an annual parallax shift of , is located roughly 730 light years from the Sun. It is a member of the Perseus OB3 association, which includes the Alpha Persei Cluster.
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14 Sagittae is a binary star system in the equatorial constellation of Aquila. 14 Sagittae is the Flamsteed designation. It appears as a sixth magnitude star, near the lower limit of visibility to the naked eye, having an apparent visual magnitude of 5.89. The system is located 660 light years away, as determined from its annual parallax shift of .
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HU Delphini, also known as Gliese 791.2, is a star system in the constellation of Delphinus. Its apparent magnitude is 13.07. With a trigonometric parallax of 113.4 ± 0.2 mas, it is about 28.76 light-years (8.82 parsecs) away from the Solar System. HU Delphini is a binary star with a well-defined period of 538.6 days.
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ADS 7251 is a binary star system 6.16 ±0.02 parsecs (20.09 ±0.07 light years) from the Sun. Both are of nearly equal brightness, but ADS 7251 A, which is 0.06 magnitudes (1.2 times) brighter than ADS 7251 B, is a red dwarf of spectral type M0.0. The latter is spectral type K7.0 and slightly further away.
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HD 83446 is a probable astrometric binary star system in the constellation Vela. It is visible to the naked eye with an apparent visual magnitude of 4.34. Based upon an annual parallax shift of , it is located 107.1 light years from the Sun. The system is moving further away with a heliocentric radial velocity of +18 km/s.
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53 Aurigae is a binary star system in the northern constellation of Auriga. It is visible to the naked eye as a dim star with a combined apparent visual magnitude of 5.74. Parallax estimates put it at a distance of away. The system is receding from the Earth with a heliocentric radial velocity of 13 km/s.
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Gamma Boötis (γ Boötis, abbreviated Gamma Boo, γ Boo) is a binary star in the constellation of Boötes. It is a Delta Scuti type variable star with a period of 1.13 hours. Its brightness varies from magnitude +3.02 to +3.07. Based on parallax measurements obtained during the Hipparcos mission, it is approximately 85 light-years distant from the Sun.
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Rho Aurigae (ρ Aur, ρ Aurigae) is the Bayer designation for a binary star system in the northern constellation of Auriga. It is faintly visible to the naked eye with an apparent visual magnitude of +5.22. Judging by parallax measurements, this system is approximately distant from the Earth, give or take a 30 light-year margin of error.
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2 Andromedae, abbreviated 2 And, is a binary star system in the northern constellation of Andromeda. 2 Andromedae is the Flamsteed designation. It is a faint star system but visible to the naked eye with a combined apparent visual magnitude of 5.09. Based upon an annual parallax shift of , it is located 420 light years away.
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10 Arietis is a binary star system in the northern constellation of Aries. 10 Arietis is the Flamsteed designation. It is visible to the naked eye as a dim, yellow-white hued star with a combined apparent visual magnitude of 5.63. Based upon parallax measurements, it is located around 159 light years away from the Sun.
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64 Arietis is a possible binary star system in the northern constellation of Aries. 64 Arietis is the Flamsteed designation. It is faintly visible to the naked eye as a dim, orange-hued star with an apparent visual magnitude of +5.67. Based upon an annual parallax shift of , this star is approximately distant from the Sun.
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86 Aquarii (abbreviated 86 Aqr) is a binary star system in the equatorial constellation of Aquarius. 86 Aquarii is the Flamsteed designation, though it also bears the Bayer designation c1 Aquarii. It is faint but visible to the naked eye with an apparent visual magnitude of +4.47. Based upon parallax measurements, the distance to this star is about .
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10 Andromedae, abbreviated 10 And, is an astrometric binary star system in the northern constellation of Andromeda. 10 Andromedae is the Flamsteed designation. It has an apparent visual magnitude of approximately 5.81, which means it is faintly visible to the naked eye. Based upon an annual parallax shift of , it is located 492 light years away.
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59 Andromedae, abbreviated 59 And, is a sixth-magnitude binary star system in the northern constellation of Andromeda. 59 Andromedae is the Flamsteed designation. As of 2017, the pair had an angular separation of along a position angle (PA) of 36°. Compare this to a separation of along a PA of 35°, as measured in 1783.
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M39 is at a distance of about from the Sun. This cluster has an estimated mass of and a linear tidal radius of . Of the 15 brightest components, six form binary star systems with one more suspected. HD 205117 is a probable eclipsing binary system with a period of 113.2 days that varies by 0.051 in visual magnitude.
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HD 117440, also known by its Bayer designation d Centauri (d Cen), is a binary star in the constellation Centaurus. It is approximately 900 light years from Earth. Both components are yellow G-type giant stars. The primary, d Centauri A, has an apparent magnitude of +4.5, while the secondary, d Centauri B, has an apparent magnitude of +4.7.
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Kepler-47c (also known as Kepler-47(AB)-c and by its Kepler Object of Interest designation KOI-3154.02) is an exoplanet orbiting the binary star system Kepler-47, the outermost of three such planets discovered by NASA's Kepler spacecraft. The system, also involving two other exoplanets, is located about 3,400 light-years (1,060 parsecs) away.
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WD J0651+2844 is a white dwarf binary star system composed of two white dwarfs. They are approximately 120,000 km apart and complete an orbit around their barycenter in less than 13 minutes. This produces an eclipse every 6 minutes. This makes it possible to gather enough data to produce extremely accurate predictions of each future eclipse.
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LHS 6343 is a star system in the northern constellation of Lyra. It appears exceedingly faint with a combined apparent magnitude of 13.435. Based on its stellar properties, the system is thought to be about 119.4 light-years (36.6 parsecs) away. LHS 6343 is a binary star with two red dwarfs, designated LHS 6343 A and B, respectively.
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Epsilon Aquilae (ε Aql, ε Aquilae) is the Bayer designation for a binary star in the equatorial constellation of Aquila. It has an apparent visual magnitude of 4.02 and is visible to the naked eye. Based upon an annual parallax of 21.05 mas, Epsilon Aquilae lies at a distance of approximately from Earth. This is a spectroscopic binary system.
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41 Capricorni is a binary star system in the southern constellation of Capricornus. It is faintly visible to the naked eye with an apparent visual magnitude of +5.24. The distance to this star, based upon an annual parallax shift of , is around 171 light years. It is moving closer with a heliocentric radial velocity of −45 km/s.
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Nu Andromedae (Nu And, ν Andromedae, ν And) is a binary star in the constellation Andromeda. The system has an apparent visual magnitude of 4.5, which is bright enough to be seen with the naked eye. It is approximately from Earth. Situated just over a degree to the west of this star is the Andromeda Galaxy.
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Kepler-47b (also known as Kepler-47 (AB) b and by its Kepler Object of Interest designation KOI-3154.01) is an exoplanet orbiting the binary star system Kepler-47, the innermost of three such planets discovered by NASA's Kepler spacecraft. The system, also involving two other exoplanets, is located about 3,400 light-years (1,060 parsecs) away.
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Hen 2-428 is a planetary nebula with a binary double white dwarf system core. This core star system is the first discovered candidate for Type Ia supernova through binary white dwarf merger process. At the time of its discovery, the star system at the core was the heaviest known double white dwarf binary star system.
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Kepler-35 is a binary star system in the constellation of Cygnus. These stars, called Kepler-35A and Kepler-35B have masses of 89% and 81% solar masses respectively, and both are assumed to be of spectral class G. They are separated by 0.176 AU, and complete an eccentric orbit around a common center of mass every 20.73 days.
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OGLE-TR-113 is a dim, distant magnitude 16 binary star in the star fields of the constellation Carina. Because of its distance of about 1170 light years, and location in a crowded field it was not notable in any way. Spectral type of the star is type K dwarf star, slightly cooler and less luminous than the Sun.
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Furuhjelm 46, also known as HD 155876 and Gliese 661, is a nearby binary star system, consisting of two very similar red dwarfs, located in the constellation Hercules. Furuhjelm 46 is the nearest "true" (i. e. not brown dwarf) star system in Hercules, however, there is brown dwarf in this constellation, located closer: WISE 1741+2553.
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It is a spectroscopic binary star, one in which the companion star is only known through analysis of the spectra. The spectral class of the primary is A5. Hermann Carl Vogel determined that Sheratan was a spectroscopic binary in 1903; its orbit was determined by Hans Ludendorff in 1907. It has since been studied for its eccentric orbit.
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BX Andromedae (BX And) is an eclipsing binary star in the constellation Andromeda. Its maximum apparent visual magnitude is 8.87. Within a cycle of approximately 14.6 hours, the brightness drops down to a magnitude of 9.53 during the main eclipse, and to a magnitude of 9.12 during the secondary one. It is classified as a Beta Lyrae variable.
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NGC 6881 is a planetary nebula, located in the constellation of Cygnus. It is formed of an inner nebula, estimated to be about one fifth of a light-year across, and symmetrical structure that spread out about one light-year from one tip to the other. The symmetry could be due to a binary star at the nebula's centre.
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There are several dimmer variable stars in Hercules. 30 Herculis, also called g Herculis, is a semiregular red giant with a period of 3 months. 361 light-years from Earth, it has a minimum magnitude of 6.3 and a maximum magnitude of 4.3. 68 Herculis, also called u Herculis, is a Beta Lyrae-type eclipsing binary star.
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Her X-1 is the prototype for the massive X-ray binaries although it falls on the borderline, , between high- and low-mass X-ray binaries. An intermediate-mass X-ray binary (IMXB) is a binary star system where one of the components is a neutron star or a black hole. The other component is an intermediate mass star.
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A contact binary is a type of binary star in which both components of the binary fill their Roche lobes. The uppermost part of the stellar atmospheres forms a common envelope that surrounds both stars. As the friction of the envelope brakes the orbital motion, the stars may eventually merge. W Ursae Majoris is an example.
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15 Sagittarii is a blue-hued binary star system in the southern zodiac constellation of Sagittarius. The estimated distance based upon photometry is around . It is faintly visible to the naked eye with an apparent visual magnitude of 5.37. The system is moving closer to the Sun with a heliocentric radial velocity of around −6 km/s.
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HD 213240 is a possible binary star system in the constellation Grus. It has an apparent visual magnitude of 6.81, which lies below the limit of visibility for normal human sight. The system is located at a distance of 133.5 light years from the Sun based on parallax. The primary has an absolute magnitude of 3.77.
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6 Persei is a binary star system in the northern constellation of Andromeda. It is faintly visible to the naked eye with an apparent visual magnitude of 5.29. The system is located 182 light years from Earth, as determined from its annual parallax shift of . It is moving further away with a heliocentric radial velocity of +42 km/s.
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WASP-2 is a binary star system in the Delphinus constellation located about 500 light-years away. The primary is magnitude 12 orange dwarf star, orbited by red dwarf star on wide orbit.Precise Differential Analysis of Stellar Metallicities: Application to Solar Analogs Including 16 Cyg A and B The star system shows an infrared excess noise of unknown origin.
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KT Lupi is a visual binary star system in the constellation Lupus. It is visible to the naked eye with a combined apparent visual magnitude of 4.55. As of 1983, the pair had an angular separation of . Based upon an annual parallax shift of as seen from Earth's orbit, it is located 430 light years from the Sun.
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2 Lyncis is a binary star system in the northern constellation Lynx. It is visible to the naked eye, having an apparent visual magnitude of 4.44. The distance to this system, judging by an annual parallax shift of , is around 157 light years. It is moving closer to the Sun with a heliocentric radial velocity of −2 km/s.
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NGC 2070 region. MK 34 is the bright isolated star to the left of the R136 cluster in the righthand panel. Melnick 34 is a binary star with an orbital period of 155 days. It shows high x-ray luminosity characteristic of colliding-wind binaries, and periodic variations in luminosity, spectral absorption, and the x-ray brightness.
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Gamma Delphini, Latinized from γ Delphini, is a binary star system approximately 101 light-years away in the constellation of Delphinus. The star marks one corner of the asterism "Job's Coffin". It is one of the best known double stars in the sky, consisting of a fourth magnitude orange subgiant and a fifth magnitude yellow-white dwarf.
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HD 125628 is a binary star system in the constellation Centaurus. It is faintly visible to the naked eye with a combined apparent visual magnitude of 4.76. The distance to this system is approximately 380 light years based on parallax. It is drifting further away from the Sun with a radial velocity of +15 km/s.
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HD 126128/9 is a triple star in the northern constellation of Boötes. Two of the components (HD 126128) form a binary star system with an orbital period of 39.5 years and an eccentricity of 0.25. The third component (HD 126129), and the brightest member of the trio, lies at an angular separation of 6.250″ from the other two.
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Beta Leonis Minoris (Beta LMi, β Leonis Minoris, β LMi) is a binary star in the constellation of Leo Minor. It has an overall apparent visual magnitude of approximately 4.2. Although it is the only star in Leo Minor with a Bayer designation, it is only the second brightest star in the constellation (the brightest is 46 Leonis Minoris).
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HD 8673 is a binary star in the northern constellation of Andromeda. It has an apparent magnitude and absolute magnitude of 6.34 and 3.56 respectively. Based upon an annual parallax shift of , the system is located around 123.6 light years away. The system is moving further from the Earth with a heliocentric radial velocity of +19 km/s.
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In 1989 (and 1999 ) this scenario was extended to binary neutron star mergers (a binary star system of two neutron stars that collide). After preliminary identification of these sites, the scenario was confirmed in GW170817. Current astrophysical models suggest that a single neutron star merger event may have generated between 3 and 13 Earth masses of gold.
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The nearest known white dwarf is Sirius B, at 8.6 light years, the smaller component of the Sirius binary star. There are currently thought to be eight white dwarfs among the hundred star systems nearest the Sun. The unusual faintness of white dwarfs was first recognized in 1910. The name white dwarf was coined by Willem Luyten in 1922.
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Iota Virginis (ι Virginis, abbreviated Iota Vir, ι Vir) is a binary star in the constellation of Virgo. Its apparent magnitude is 4.08. Based on its parallax, it is assumed to be relatively nearby, at 72.5 light-years (22.24 parsecs). Its two components are designated Iota Virginis A (officially named Syrma , the traditional name for the system) and B.
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HD 24496 is a 7th magnitude G-type wide binary star and M-type located approximately 67 light years away in the constellation Taurus. This star is smaller, cooler, fainter, and less massive than our Sun. Also its metal content is just 2% greater than the Sun. In 2009, a gas giant planet was discovered of HD 24496 A.
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HR 2554 has two components in orbit around each other, making it a binary star. The semi-major axis of the secondary's orbit is 2.17 arcseconds. The two components regularly eclipse each other, making A Carinae a variable star. Its brightness varies by 0.06 magnitudes with a period equal to its orbital period of 195 days.
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Mu Ursae Majoris (μ Ursae Majoris, abbreviated Mu UMa, μ UMa), formally named Tania Australis , is a binary star in the constellation of Ursa Major. An apparent visual magnitude of +3.06 places it among the brighter members of the constellation. Parallax measurements give an estimated distance of roughly from the Sun, with a margin of error of 4%.
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Kappa Ursae Majoris (κ Ursae Majoris, abbreviated Kappa UMa, κ UMa) is a binary star in the constellation of Ursa Major. With a combined apparent magnitude of +3.60, the system is approximately 358 light-years from Earth. The two components are designated Kappa Ursae Majoris A (officially named Alkaphrah , a traditional name of the system) and B.
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XO-2 is a binary star. It consists of two components: XO-2S (Also known as XO-2A) and XO-2N (Also known as XO-2B). This system is located approximately 500 light-years away from Earth in the Lynx constellation. Both of these stars are slightly cooler than the Sun and are nearly identical to each other.
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Zeta Crucis, Latinized from ζ Crucis, is a binary star system in the southern constellation of Crux. It is visible to the naked eye with an apparent magnitude of 4.06m. ζ Crucis is located at about 360 light-years from the Sun. It is a member of the Lower Centaurus Crux subgroup of the Scorpius-Centaurus Association.
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Theta2 Crucis, Latinized from θ2 Crucis, is a spectroscopic binary star in the constellation Crux. This pair of stars complete an orbit every 3.4280 days and they have a low orbital eccentricity that is close to 0.0. Theta2 Crucis is located at about 750 light-years from the Sun. The system has a combined mean apparent magnitude of +4.72m.
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TY Pyxidis is an eclipsing binary star in the constellation Pyxis. The apparent magnitude ranges from 6.85 to 7.5 over 3.2 days. The two components are both of spectral type G5IV, have a mass of 1.2 solar masses and revolve around each other every 3.2 days. Each star is around 2.2 times the diameter of the Sun.
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WZ Cephei is an eclipsing binary star of W Ursae Majoris-type in the constellation of Cepheus, located 880 light years away from the Sun. The stars orbit around a common orbital barycenter every 0.41744 days (slightly over 10 hours). Timing analyses have revealed the possible presence of a third low- mass stellar companion in a wide orbit.
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Zeta Phoenicis (ζ Phoenicis, abbreviated Zet Phe, ζ Phe) is a multiple star system in the constellation of Phoenix. It is visible to the naked eye. Based upon parallax measurements made by the Hipparcos spacecraft, it is located some 300 light years (92 parsecs) away. Zeta Phoenicis A is itself an Algol- type eclipsing binary star.
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The primary is actually two very similar white main sequence stars that are 5.3 AU distant from each other and the secondary is two small main sequence stars, most likely red dwarfs, that are 600 AU from the main pair. Hence the system is a quadruple one. Zeta Cancri or Tegmine ("the shell") is a multiple star system that contains at least four stars located 82 light-years from Earth. The two brightest components are a binary star with an orbital period of 1100 years; the brighter component is a yellow-hued binary pair and the dimmer component is a yellow-hued star of magnitude 6.2. The brighter component is itself a binary star with a period of 59.6 years; its primary is of magnitude 5.6 and its secondary is of magnitude 6.0.
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Eta Sagittarii (Eta Sgr, η Sagittarii, η Sgr) is a binary star system in the southern zodiac constellation of Sagittarius. Based upon parallax measurements, it is located at a distance of from Earth. It was formerly known as Beta Telescopii (β Tel). In India, where part of the constellation of Sagittarius represents an Elephant, this star forms the creature's tail.
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Trimble, 4. King worked with him until she was accepted into the Berlin Academy of Fine Arts in 1937, when she was 21, one of only three non-Aryan students there (all women).Jane Eckett: "Binary Star: Inge and Grahame King", 3, n.4; also 4, n.8, which refers to records of the "Vereinigte Staatsschulen für freie und angewandte Kunst".
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Zeta Volantis (ζ Vol, ζ Volantis) is a binary star system in the southern constellation of Volans. It has an apparent visual magnitude of 3.93, which is bright enough to be seen with the naked eye. Based upon parallax measurements, it is approximately 141 light years from the Sun. The companion is a magnitude 9.7 star at an angular separation of 16.7″.
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DS Tucanae (HD 222259) is a binary star system in the constellation of Tucana. It has an apparent visual magnitude of 8.5, and is a RS Canum Venaticorum variable. The system is notable for being young as a member of the 45 Myr old Tucana-Horologium moving group and for the primary star hosting the confirmed exoplanet DS Tucanae Ab, discovered by TESS.
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Sarah Gerard is an American writer of fiction and nonfiction. She recently worked for Bomb Magazine. She is the author of a novel, Binary Star, published in 2015 by Two Dollar Radio. It was a finalist for the Los Angeles Times Art Seidenbaum Award for First Fiction, and was listed as a best book of the year by NPR and Vanity Fair.
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HR 7578 (also known as V4200 Sagittarii) is a binary star in the constellation of Sagittarius. Their combined apparent magnitude is 6.18. Parallax measurements by the Gaia spacecraft put the system at 46.01 light-years (14.107 parsecs) away, making this a nearby system. The two stars of HR 7578 are fairly old, older than the Pleiades but possibly younger than the Hyades.
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KOI-81 is an eclipsing binary star in the constellation of Cygnus. The primary star is a late B-type or early A-type main-sequence star with a temperature of . It lies in the field of view of the Kepler Mission and was determined to have an object in orbit around it which is smaller and hotter than the main star.
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12 Persei (12 Per) is a double-lined spectroscopic binary star system in the northern constellation Perseus. Its combined apparent magnitude is 4.94, which means it can be viewed with the naked eye. Based upon parallax measurements, this system is about 79 light years away from the Sun. The magnitude difference between the two components is estimated to be 0.51.
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33 Piscium is a binary star system in the zodiac constellation of Pisces. It is visible to the naked eye with an apparent visual magnitude of 4.61. The distance to this system, as determined from an annual parallax shift of , is about 129 light years. It is moving closer to the Sun with a heliocentric radial velocity of −6.6 km/s.
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HD 74180 is a binary star in the constellation Vela. It is approximately 3,200 light years from Earth. The primary component is a yellow-white F-type supergiant with a mean apparent magnitude of +3.81, with a 10th magnitude companion 37.5 arcseconds distant. b Velorum has been classified as a suspected α Cygni variable star which varies by only 0.06 magnitude.
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Gliese 673 is an orange dwarf star in the constellation Ophiuchus. It has a stellar classification of K7V. Main sequence stars with this spectra have a mass in the range of 60-70% of solar mass () (comparable to the members of the binary star system 61 Cygni). This star is relatively near our Sun at a distance of about 25 light years.
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DV Aquarii is a binary star system in the zodiac constellation of Aquarius. It has a peak apparent visual magnitude of 5.89, which is bright enough to be visible to the naked eye. The distance can be estimated from its annual parallax shift of , yielding a separation of 291 light years. This is a detached eclipsing binary system of the Beta Lyrae type.
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In 1918, Maury returned to Harvard College Observatory as an adjunct professor. With Pickering's successor Harlow Shapley she was given credit for her work, which was published under her own name. She stayed in the observatory until her retirement in 1948. Her work summarizing many years of research on the spectroscopic analysis of the binary star Beta Lyrae was published in 1933.
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HD 115404 is a binary star system located in the constellation Coma Berenices. Parallax measurements made by Hipparcos put the system at 36 light-years, or 11 parsecs, away. The combined apparent magnitude of the system is 6.52, with the magnitudes of the components being 6.66 and 9.50. The primary component, designated A, is a K-type main sequence star.
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Gamma Coronae Australis (γ CrA), is a binary star located in the constellation Corona Australis. The system has a combined apparent visual magnitude of 4.20, making it faintly visible to the naked eye. It is located 56.4 light-years (17.3 parsecs) from the Sun, based on its parallax. Gamma Coronae Australis is a member of the Milky Way's thin disk.
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AT Microscopii is a binary star system located at a distance of from the Sun in the constellation of Microscopium. Both members are flare stars, meaning they are red dwarf stars that undergo random eruptions that increase their brightness. This pair lies physically near the red dwarf star AU Microscopii, which may mean they form a wide triple star system.
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The roman numerals indicate a luminosity class of bright giant. Most such stars are found in binary star systems, but this appears to be an exception as no companion has been discovered. Evolved stars with Am-like peculiarities of abundance have come to be known as ρ Puppis stars. The star's metallicity is more than double that in the Sun.
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Omicron Puppis (ο Puppis) is candidate binary star system in the southern constellation of Puppis. It is visible to the naked eye, having a combined apparent visual magnitude of +4.48. Based upon an annual parallax shift of 2.30 mas as seen from Earth, it is located roughly 1,400 light years from the Sun. This is a suspected close spectroscopic binary system.
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HD 106515 is a binary star (and currently visual triple system) in the constellation of Virgo. The A and B stars are both K-type main-sequence stars. The two are gravitationally bound and separated at 310 AU. The binary semimajor axis is 390 AU. The third star in the visual triple, BD−06° 3533, is a physically unrelated background star.
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Finally, the 'p' shows some peculiarity in the spectrum. It is classified as a Gamma Cassiopeiae type variable star and its brightness varies from magnitude +5.43 to +5.61. This is a runaway star with a peculiar velocity of . Because it is a binary star system, it was most likely not turned into a runaway system as the result of a supernova explosion.
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HD 199942 is a binary star system in the northern constellation of Equuleus. It is faintly visible to the naked eye with an apparent visual magnitude of 5.98. The system is located at a distance of approximately 184 light years based on parallax, and it has an absolute magnitude of 1.59. It is drifting closer with a radial velocity of −26 km/s.
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HD 91324 is a likely binary star system in the southern constellation of Vela. It is visible to the naked eye with an apparent visual magnitude of 4.89. The distance to HD 91324, as determined from its annual parallax shift of , is 71.5 light years. It is moving further from the Earth with a heliocentric radial velocity of +21 km/s.
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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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KX Andromedae (often abbreviated to KX And) is a spectroscopic binary star in the constellation Andromeda. Its apparent visual magnitude varies between 6.88 and 7.28. The primary component of the KX Andromedae system is a Be star with a spectral classification B3pe. The secondary star is difficult to detect in the spectrum, but has been given a K1III spectral type.
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132 Tauri is a binary star system in the constellation Taurus. It is faintly visible to the naked eye with an apparent visual magnitude of 4.89. Based upon a poorly-constrained annual parallax shift of , it is located roughly 360 light years from the Sun. The system is moving further away with a heliocentric radial velocity of +16 km/s.
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27 Arietis is a binary star system in the northern constellation of Aries. 27 Arietis is the Flamsteed designation. It is a dim, yellow-hued star that is close to the lower limit of what can be viewed with the naked eye, having an apparent visual magnitude is 6.21. The annual parallax shift of corresponds to a physical distance of approximately from Earth.
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AR Aurigae (AR Aur), also known by its Flamsteed designation 17 Aurigae, is a binary star in the constellation Auriga. Based on parallax measurements made by the Hipparcos spacecraft, it is approximately 400 light-years from Earth. Both components are blue-white B-type main-sequence stars that do not fill their Roche lobes. The system has a mean apparent magnitude of +6.15.
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T Pyxidis (T Pyx)According to the Argelander system of nomenclature for variable stars, the initial letter is an R, and the counter progresses alphabetically. Thus, T Pyx is the third variable star in the constellation Pyx. is a recurrent nova and nova remnant in the constellation Pyxis. It is a binary star system and its distance is estimated at about from Earth.
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21 Arietis (abbreviated 21 Ari) is a binary star system in the northern constellation of Aries. 21 Arietis is the Flamsteed designation. It has a combined apparent visual magnitude is 5.57; the brighter member is magnitude 6.40 while the fainter star is magnitude 6.48. The distance to this star system, based upon an annual parallax shift of 19.58 mas, is .
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97 Aquarii (abbreviated 97 Aqr) is a binary star system in the equatorial constellation of Aquarius. 97 Aquarii is the Flamsteed designation. The combined apparent visual magnitude of the system is 5.20; the brighter star is magnitude 5.59 while the companion is magnitude 6.72. Based upon an annual parallax shift of 15.30 milliarcseconds, this system is at a distance of around from Earth.
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36 Andromedae is a visual binary star system in the northern constellation of Andromeda. The designation is from the star catalogue of English astronomer John Flamsteed, first published in 1712. It is faintly visible to the naked eye with an apparent visual magnitude of 5.45. An annual parallax shift of 26.33 mas yields a distance estimate of about 124 light years.
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C3 Centauri is a suspected astrometric binary star system in the southern constellation of Centaurus. It has an orange hue and is dimly visible to the naked eye with an apparent visual magnitude of +5.46. The distance to this object is approximately 342 light years based on parallax. It is a member of the Hyades Stream of co-moving stars.
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Spectrographic images taken at the Cape Observatory between 1921 and 1923 showed this star has a variable radial velocity, which indicated this is a single-lined spectroscopic binary star system. The pair have an orbital period of 9.94 days and an eccentricity of about 0.2. The primary component has received a number of different stellar classifications. For example, Jaschek et al.
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31 Crateris is a binary star system in the constellation Corvus. Varying between apparent magnitudes 5.19 and 5.23 over 1.48 days, it has the variable star designation of TY Corvi. It is actually a remote system with a hot blue- white star of spectral type B1.5V and a companion about which little is known. The two stars orbit each other every 2.9631 days.
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Doppler imaging was first used to map chemical peculiarities on the surface of Ap stars. For mapping starspots it was first used by Steven Vogt and Donald Penrod in 1983, when they demonstrated that signatures of starspots were observable in the line profiles of the active binary star HR 1099 (V711 Tau); from this they could derive an image of the stellar surface.
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Gliese 752 is a binary star system in the Aquila constellation. This system is relatively nearby, at a distance of about 19 light years. This system consists of two M-type stars. The primary star is the magnitude 9 Gliese (GJ) 752 A. The secondary star is the dim magnitude 17 Gliese (GJ) 752 B, more commonly referred to as VB 10.
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Alcor is a binary star system in the constellation of Ursa Major. It is the fainter companion of Mizar, the two stars forming a naked eye double in the handle of the Big Dipper (or Plough) asterism in the constellation of Ursa Major. The two both lie about 83 light-years away from the Sun, as measured by the Hipparcos astrometry satellite.
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HD 29573 is a binary star system in the constellation Eridanus. It has a combined apparent visual magnitude of 4.99, making it visible to the naked eye. Based upon an annual parallax shift of , it is located 217 light years from the Sun. The system is moving further away from Earth with a heliocentric radial velocity of +3 km/s.
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AU Microscopii is a member of the β Pictoris moving group. AU Microscopii may be gravitationally bound to the binary star system AT Microscopii. AU Microscopii has been observed in every part of the electromagnetic spectrum from radio to X-ray and is known to undergo flaring activity at all these wavelengths. Its flaring behaviour was first identified in 1973.
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T Cygni is a binary star system in the northern constellation of Cygnus. It is a faint system but visible to the naked eye with a combined apparent visual magnitude of 4.93. Based upon an annual Parallax shift of , it is located 387 light years away. It is moving closer to the Earth with a heliocentric radial velocity of −24 km/s.
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22 Cygni is a binary star system in the northern constellation of Cygnus. It is visible to the naked eye as a faint, blue-white hued star with an apparent visual magnitude of 4.95. The annual shift of yields a distance estimate of around 1,070 light years. It is moving closer to the Earth with a heliocentric radial velocity of −15 km/s.
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Psi1 Piscium (Psi1 Psc, ψ1 Piscium, ψ1 Psc) is binary star in constellation of Pisces. It is approximately 280 light years from Earth, based on its parallax. The two components of Psi1 Piscium are both A-type main-sequence stars. The primary has an apparent magnitude of 5.273, while the secondary is slightly dimmer, with an apparent magnitude of 5.455.
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It has a projected rotational velocity of 255 km/s, resulting in an equatorial bulge with a radius 13% larger than the polar radius. It has a magnitude 9.5 companion G-type main sequence star that may form a binary star system with Delta Arae. There is a 12th magnitude optical companion located 47.4 arcseconds away along a position angle of 313°.
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Theta Andromedae (θ And, θ Andromedae) is the Bayer designation for a binary star in the constellation Andromeda. It is approximately from Earth, with a visual magnitude of 4.6. On the Bortle Dark-Sky Scale, this makes it visible to the naked eye from outside urban regions. Theta Andromedae is a white A-type main sequence dwarf with an apparent magnitude of +4.61.
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HD 176051 is a spectroscopic binary star system approximately 49 light years away from Earth in the constellation Lyra. The pair orbit with a period of 22,423 days (61.4 years) and an eccentricity of 0.25. Compared to the Sun, they have a somewhat lower proportion of elements more massive than helium. Their individual masses are estimated at 1.07 and 0.71 solar masses ().
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42 Capricorni is a binary star system in the zodiac constellation of Capricornus. It has a combined apparent visual magnitude of 5.18, indicating it is faintly visible to the naked eye. An annual parallax shift of 30.09 mas yields a distance estimate of about 108 light years. The system is moving closer to the Sun with a radial velocity of −1.2 km/s.
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Rho Capricorni (ρ Cap, ρ Capricorni) is a binary star in the constellation Capricornus. Sometimes, this star is called by the name Bos, meaning the cow in Latin. In Chinese, (), meaning Ox (asterism), refers to an asterism consisting of β Capricorni, α2 Capricorni, ξ2 Capricorni, π Capricorni, ο Capricorni and ρ Capricorni. 中國星座神話, written by 陳久金.
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This star has 55% more mass than the Sun. It shines with 6.6 times the Sun's luminosity at an effective temperature of 7,132 K. This heat gives it the yellow-white glow of an F-type star. It has a faint companion located 31 arcseconds away with an apparent magnitude of +11.3. Most likely this pair form a binary star system.
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HD 30453 is a binary star system in the northern constellation of Auriga. It is visible to the naked eye with an apparent visual magnitude of 5.86. The system is located at a distance of approximately 334 light years from the Sun based on parallax. It is drifting further away from the Sun with a radial velocity of 16.65 km/s.
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Current space telescopes, including NASA's Hubble Space Telescope, can accurately measure mass for some types of stars, but not all. Estimates put the range for stellar mass somewhere between 8% the mass of the Sun and in excess of 60 times the mass of the Sun. The entire study was to focus on binary star systems, stars coupled through a mutual gravitational attraction.
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Her main research interests can be divided into three groups: computational astrophysics, stellar astrophysics, and exoplanets and brown dwarfs. Among the investigations she carried out, the speciality of Richards’ research are binary stars. A binary star is a system formed by two stars that were born at the same time which orbit around a common center. The stars, however, mature at different rates.
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Omicron Cephei, Latinized from ο Cephei, is a binary star in the constellation of Cepheus. It consists of a less massive F-type main sequence star in orbit with a more massive G-type giant star. The overall apparent visual magnitude of the system is 4.75. The pair was first determined to be binary by F. G. W. Struve in 1832.
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Gliese 412 is a pair of stars that share a common proper motion through space and are thought to form a binary star system. The pair have an angular separation of 31.4″ at a position angle of 126.1°. They are located 15.8 light years distant from the Sun in the constellation Ursa Major. Both components are relatively dim red dwarf stars.
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HD 3346, also known as V428 Andromedae, is a binary star system in the northern constellation of Andromeda. It is a dim star but visible to the naked eye under suitable viewing conditions, having an apparent visual magnitude of 5.14. The distance to HD 3346 can be determined from its annual parallax shift of . This yields a range of about 660 light year.
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U Geminorum (U Gem), in the constellation Gemini, is an archetypal example of a dwarf nova. The binary star system consists of a white dwarf closely orbiting a red dwarf. Every few months it undergoes an outburst that greatly increases its brightness. The dwarf nova class of variable stars are often referred to as U Geminorum variables after this star.
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HR 7484 (V1143 Cyg) is a binary star system in the northern constellation of Cygnus. It is dimly visible to the naked eye under good viewing conditions, having an apparent visual magnitude of 5.89. Based upon an annual parallax shift of 24.71, it is located 132 light years away. The system is moving closer with a heliocentric radial velocity of −14 km/s.
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AB Andromedae (AB And) is a binary star in the constellation Andromeda. Its maximum apparent visual magnitude is 9.49 but shows a variation in brightness down to a magnitude of 10.46 in a periodic cycle of roughly 8 hours. The observed variability is typical of W Ursae Majoris variable stars, so the two stars in this system form a contact binary.
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HD 195019 b is an exoplanet orbiting around HD 195019 in the binary star system. It has a minimum mass of 3.7 MJ. It orbits very close to the star. Like many planets at close distance, its orbit is circular, even more circular or less eccentric than Earth. It takes 437 hours to orbit with velocity of 83.24 kilometers per second.
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AK Scorpii is a Herbig Ae/Be star and spectroscopic binary star about 459 light-years distant in the constellation Scorpius. The star belongs to the nearby Upper Centaurus–Lupus star-forming region and the star is actively accreting material. The binary is surrounded by a circumbinary disk that was imaged with VLT/SPHERE in scattered light and with ALMA.
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Xi Draconis (ξ Draconis, abbreviated Xi Dra, ξ Dra) is a double or binary star in the northern circumpolar constellation of Draco. It has an apparent visual magnitude of 3.75. Based upon parallax measurements, it is located at a distance of from the Sun. At this distance, the apparent magnitude is diminished by 0.03 from extinction caused by intervening gas and dust.
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It is in reality a remote binary star system with a hot blue-white star of spectral type B1.5V and a companion about which little is known. The two stars orbit each other every 2.9631 days. The primary is possibly a blue straggler of the Hyades group. The primary is around 15.5 times as massive as the Sun and 52262 times as luminous.
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Ultraviolet rays emitted from WR 136's hot surface cause the shell to glow. There is some evidence WR 136 may be a binary star. Its companion would be a low-mass star of spectral classification K or M that would complete an orbit around the Wolf-Rayet star each 5.13 days, being the progenitor of a low-mass X-ray binary system.
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Consider a binary star system. This consists of two objects, of mass m_1 and m_2, orbiting around their centre of mass. m_1 has position vector r_1 and orbital velocity v_1, and m_2 has position vector r_2 and orbital velocity v_2 relative to the centre of mass. The separation between the two stars is denoted r, and is assumed to be constant.
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The orange main-sequence star is the primary of magnitude 4.4, and the white secondary of magnitude 9.5 is the most easily visible white dwarf. The red dwarf, of magnitude 11, orbits the white dwarf every 250 years. The 40 Eridani system is 16 light-years from Earth. p Eridani is a binary star with two orange components, 27 light-years from Earth.
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The first six weeks of data revealed five previously unknown planets, all very close to their stars. Among the notable results are one of the least dense planets yet found, two low-mass white dwarfs that were initially reported as being members of a new class of stellar objects, and Kepler-16b, a well-characterized planet orbiting a binary star.
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UZ Fornacis (abbreviated as UZ For) is a binary star in the constellation of Fornax. It appears exceedingly faint with a maximum apparent magnitude 17.0. Its distance, as measured by Gaia using the parallax method, is about 780 light-years (240 parsecs). The system consists of two stars, a white dwarf and a red dwarf, in close orbit around each other.
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12 Nevertheless, objects as small as 8 Jupiter masses have been called a brown dwarf.Discovery of a Planetary-Mass Brown Dwarf with a Circumstellar Disk, Luhman, et al., 2005 A substellar companion is thought to exist in the binary star system SDSS 1212.Detection of Substellar Companion in Interacting Binary Substellar companions have been confirmed by analyzing astrometric data from Hipparcos.
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66 Eridani is a binary star in the constellation of Eridanus. The combined apparent magnitude of the system is 5.12 on average. Parallax measurements by Hipparcos put the system at some 309 light-years (95 parsecs) away. This is a spectroscopic binary: the two stars cannot be individually resolved, but periodic Doppler shifts in its spectrum mean there must be orbital motion.
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HD 151613 is a binary star system in the northern circumpolar constellation of Draco. It is visible to the naked eye with an apparent visual magnitude of 4.84. The distance to this star, as estimated from its annual parallax shift of , is 83 light years. It is moving closer to the Earth with a heliocentric radial velocity of −2 km/s.
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HD 217382 is a suspected binary star system in the northern circumpolar constellation of Cepheus. It is faintly visible to the naked eye with an apparent visual magnitude of 4.70. The distance to HD 217382 is around 319 light years, as determined from an annual parallax shift of . The system is moving further away with a heliocentric radial velocity of +2.6 km/s.
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U Lacertae is a spectroscopic binary star in the constellation Lacerta. Despite being in the constellation of Lacerta, U Lacertae is considered to be a member of the Cepheus OB1 association. It has been listed as a member of the open cluster ASCC 123. U Lacertae is a VV Cephei binary consisting of a red supergiant and a small hot companion.
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Delta Trianguli (Delta Tri, δ Trianguli, δ Tri) is a spectroscopic binary star system approximately away in the constellation of Triangulum. The primary star is a yellow dwarf, while the secondary star is thought to be an orange dwarf. It has an apparent magnitude of +4.87 and forms an optical (line-of-sight) triple with Gamma Trianguli and 7 Trianguli.
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Delta Capricorni A is an Algol-type eclipsing binary star, with an orbital period of 1.022768 days and an inclination close to the line of sight from the Earth. The peak apparent visual magnitude of the pair is 2.81. During an eclipse of the primary, this magnitude drops by 0.24. When the primary is eclipsing the secondary, the magnitude decreases by 0.09.
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Both components of the binary star are white A-type main sequence dwarfs. They have apparent magnitudes of +4.2 and +4.5. The orbital period of the binary is 35.6 years (13,007.2 days), and the two stars are separated by 0.18 arcseconds. An infrared excess indicates a debris disk with a mean temperature of 165 K is orbiting the primary at a separation of .
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Observational studies of their radial velocity suggested that all barium stars are binary stars. Observations in the ultraviolet using International Ultraviolet Explorer detected white dwarfs in some barium star systems. Barium stars are believed to be the result of mass transfer in a binary star system. The mass transfer occurred when the now-observed giant star was on the main sequence.
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X Caeli, or Gamma2 Caeli, is a binary star system in the southern constellation of Caelum. It is barely visible to the naked eye with an apparent visual magnitude of 6.32. based upon an annual parallax shift of , it is located 341 light years from Earth. The system is moving further away with a heliocentric radial velocity of +6 km/s.
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HD 42818 is a suspected astrometric binary star system in the northern circumpolar constellation of Camelopardalis. It is visible to the naked eye with an apparent visual magnitude of +4.76. Based upon an annual parallax shift of as seen from Earth's orbit, it is located some 175 light years away. The system appears to be moving closer with a heliocentric radial velocity of .
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It has a period of 13 months and a diameter of between 329 to 500 solar diameters. There are several prominent double stars and binary stars in Cepheus. Omicron Cephei is a binary star with a period of 800 years. The system, 211 light-years from Earth, consists of an orange-hued giant primary of magnitude 4.9 and a secondary of magnitude 7.1.
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Stellar multiplicity increases with stellar mass: the likelihood of stars being in multiple systems is about 25% for red dwarfs, about 45% for Sun-like stars, and rises to about 80% for the most massive stars. Of the multiple stars about 75% are binaries and the rest are higher-order multiplicities.Stellar Multiplicity, Gaspard Duchêne (1,2), Adam Kraus (3) ((1) UC Berkeley, (2) Institut de Planétologie et d'Astrophysique de Grenoble, (3) Harvard- Smithsonian CfA), (Submitted on 12 Mar 2013) More than one hundred planets have been discovered orbiting one member of a binary star system (e.g. 55 Cancri, possibly Alpha Centauri Bb),BINARY CATALOGUE OF EXOPLANETS , Maintained by Richard Schwarz], retrieved 28 Sept 2013 and several circumbinary planets have been discovered which orbit around both members of a binary star (e.g. PSR B1620-26 b, Kepler-16b).
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KPD 1930+2752 is a binary star system including a Subdwarf B star and a probable white dwarf with relatively high mass. Due to the nature of this astronomical system, it seems like a likely candidate for a potential type Ia supernova, a type of supernova which occurs when a white dwarf star takes on enough matter to approach the Chandrasekhar limit, the point at which electron degeneracy pressure would not be enough to support its mass. However, carbon fusion would occur before this limit was reached, releasing enough energy to overcome the force of gravity holding the star together and resulting in a supernova. The total mass of the binary star system likely exceeds the Chandrasekhar limit, making this system one of the most likely candidates known to serve as a progenitor for a future type Ia supernova.
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Schematic of a binary star system with one planet on an S-type orbit and one on a P-type orbit While a number of binary star systems have been found to harbor extrasolar planets, such systems are comparatively rare compared to single star systems. Observations by the Kepler space telescope have shown that most single stars of the same type as the Sun have plenty of planets, but only one-third of binary stars do. According to theoretical simulations, even widely separated binary stars often disrupt the discs of rocky grains from which protoplanets form. On the other hand, other simulations suggest that the presence of a binary companion can actually improve the rate of planet formation within stable orbital zones by "stirring up" the protoplanetary disk, increasing the accretion rate of the protoplanets within.
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21 Sagittarii is a binary star system in the southern zodiac constellation of Sagittarius. It is visible to the naked eye as a faint point of light with a combined apparent visual magnitude of 4.81. The system is located approximately 410 light years away from the Sun based on parallax. It is moving closer to the Earth with a heliocentric radial velocity of −11.80 km/s.
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HD 256 is a binary star system in the equatorial constellation of Cetus. It has a white hue and is dimly visible to the naked eye with an apparent visual magnitude of 6.20. Based upon parallax measurements, the system is located at a distance of approximately 474 light years from the Sun. It is drifting closer with a radial velocity of −10 km/s.
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Lambda Virginis (λ Virginis, abbreviated Lambda Vir, λ Vir) is a binary star system in the zodiac constellation of Virgo. With an apparent visual magnitude of 4.5, it is bright enough to be seen with the naked eye. Based upon parallax measurements, the system is about 173 light-years away from the Sun. Its two components are designated Lambda Virginis A (formally named Khambalia ) and B.
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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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Kappa2 Sagittarii (κ2 Sagittarii) is a binary star system in the zodiac constellation of Sagittarius. It is visible to the naked eye with a combined apparent visual magnitude of +5.64. Based upon an annual parallax shift of 10.47 mas as seen from Earth, this system is located around 310 light years from the Sun. They are receding with a radial velocity of +2.6 km/s.
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6 Serpentis is a binary star system in the constellation Serpens. It has a combined apparent visual magnitude of 5.382, which is bright enough to be faintly visible to the naked eye. The distance to this system, based upon an annual parallax shift of , is about 240 light years. It is moving further from the Sun with a heliocentric radial velocity of +10 km/s.
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His research started with his PhD in relativistic cosmology, working with his supervisor George F. R. Ellis at the University of Cambridge. He also worked with Stephen Hawking. He has worked in the fields of General Relativity, binary star evolution, accretion discs and active galactic nuclei. In 2014 he received the Eddington Medal of the Royal Astronomical Society "for investigations of outstanding merit in theoretical astrophysics".
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56 Pegasi is a binary star system in the northern constellation of Pegasus. It is visible to the naked eye with a combined apparent visual magnitude of 4.74. The system is approximately 590 light years away from the Sun based on parallax, but is drifting closer with a radial velocity of −28 km/s. It is listed as a member of the Wolf 630 moving group.
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Alpha Delphini (α Delphini, abbreviated Alpha Del, α Del) is a multiple star system in the constellation of Delphinus. It consists of a binary star, designated Alpha Delphini A, together with five faint, probably optical companions, designated Alpha Delphini B, C, D, E and F. A's two components are themselves designated Alpha Delphini Aa (officially named Sualocin , the historical name for the entire system) and Ab.
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Eta Cassiopeiae (η Cassiopeiae, abbreviated Eta Cas, η Cas) is a binary star system in the northern circumpolar constellation of Cassiopeia. Its binary nature was first discovered by William Herschel in August 1779. Based upon parallax measurements, the distance to this system is from the Sun. The two components are designated Eta Cassiopeiae A (officially named Achird , the traditional name for the system) and B.
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Nu Orionis (ν Orionis) is a binary star system in the northeastern part of the constellation Orion. It should not be confused with the variable star NU Orionis. Nu Orionis has an apparent visual magnitude of 4.42, which is bright enough to be seen with the naked eye. Based upon an annual parallax shift of 0.00632 arcseconds, the distance to this system is roughly 520 light years.
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Assuming a distance of 2.2 kiloparsecs, HD 168625 is 220,000 times brighter than the Sun, having a surface temperature of 12,000 K. It is losing mass through a very strong stellar wind at a rate of roughly per year and observations realized in 2012 with the help of the VLT show it's actually a binary star, with the companion being around 4.5 magnitudes fainter than the primary.
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Beta Phoenicis (β Phoenicis, β Phe) is a binary star in the constellation Phoenix. Its apparent magnitude is 3.30, meaning that it can be seen with the naked eye (see Bortle scale). The distance to Beta Phoenicis is poorly known. The original reduction of the Hipparcos satellite's data yielded a parallax value of 16 milliarcseconds, yet its standard error was larger than the parallax value itself.
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4 Ursae Minoris is a binary star system in the northern circumpolar constellation Ursa Minor. It is faintly visible to the naked eye with an apparent visual magnitude of 4.80. Based upon an annual parallax shift of as seen from Earth's orbit, it is located roughly 460 light years from the Sun. It is moving further away with a heliocentric radial velocity of +5.9 km/s.
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83 Leonis, abbreviated 83 Leo, is a binary star system approximately 59 light- years away in the constellation of Leo (the Lion). The primary star of the system is a cool orange subgiant star, while the secondary star is an orange dwarf star. The two stars are separated by at least 515 astronomical units from each other. Both stars are presumed to be cooler than the Sun.
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ADS 16402 is a binary star system in Lacerta, around which a planet orbits with some unusual properties.Puzzling Puffy Planet, Less Dense Than Cork, Is Discovered - New York Times The Jupiter-sized planet exhibits an unexpectedly low density, about the same as cork. This planet is dubbed HAT P-1. EV Lacertae is a rapidly spinning magnitude 10 red dwarf with a strong magnetic field.
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During a globular cluster's adolescence, the process of core-collapse begins with stars near the core. However, the interactions between binary star systems prevents further collapse as the cluster approaches middle age. Finally, the central binaries are either disrupted or ejected, resulting in a tighter concentration at the core. The interaction of stars in the collapsed core region causes tight binary systems to form.
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Its name comes from the Greek word for "scorching" or "searing". Sirius is also a binary star; its companion Sirius B is a white dwarf with a magnitude of 8.4–10,000 times fainter than Sirius A to observers on Earth. The two orbit each other every 50 years. Their closest approach last occurred in 1993 and they will be at their greatest separation between 2020 and 2025.
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This is a single-lined spectroscopic binary star system that belongs to the Pleiades stream. As of 2011, the pair had a linear projected separation of . The primary component is a mercury-manganese star with a stellar classification of B8II/III. These stars are often helium- weak, but this is one of the most normal members of this group in terms of helium abundance.
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The light curve of an intermediate polar may show several types of stable periodic changes in brightness. One periodicity is related to the orbital period of the binary star system. The orbital periods of confirmed intermediate polars range from 1.4 to 48 hours, with typical values between 3 and 6 hours. A second periodic signal originates from the rotation of the white dwarf spinning on its axis.
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36 Tauri (abbreviated to 36 Tau) is a binary star in the constellation of Taurus. Parallax measurements made by the Hipparcos spacecraft put it at a distance of over 1,000 light years (350 parsecs) from Earth. The combined apparent magnitude of the system is about 5.5, meaning it can barely be seen with the naked eye, according to the Bortle scale. 36 Tauri is a spectroscopic binary.
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The earliest main sequence stars are of type A0. One of the stars in the cluster region shows extremely red colour along with blue ultraviolet colour and it could be an interacting binary star. The turnoff point is at 2.6 ±0.1 . The members show small dispersions in abundance, with the exception of Mg, which is common for clusters of rather low mass, as NGC 4815.
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Hydrogen deficiency results from stellar evolution. Over the course of a star's evolution, both the consumption of hydrogen in nuclear fusion and the removal of hydrogen layers by explosive processes can lead to a deficiency of hydrogen in its atmosphere. Detailed theoretical models are still in their infancy. Modeling of hydrogen-deficient star evolution involves either a single-star approach or a binary-star approach.
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RT Andromedae is a variable star in the constellation of Andromeda. The system is estimated to be 322 light-years (98.7 parsecs) away. RT Andromedae is classified as a RS Canum Venaticorum variable, a type of close eclipsing binary star. It varies from an apparent visual magnitude of 9.83 at minimum brightness to a magnitude of 8.97 at maximum brightness, with a period of 0.6289216 days.
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Sigma Ceti (σ Ceti) is the Bayer designation for a star in the equatorial constellation of Cetus. With an apparent visual magnitude of 4.78, it can be seen with the naked eye on a dark night. Based upon an annual parallax shift of 37.46 mas, it lies at an estimated distance of 87.1 light years from the Sun. It is a probable astrometric binary star system.
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A joint venture between the United States Naval Observatory, the Naval Research Laboratory, the Smithsonian Astrophysical Observatory, and the Massachusetts Institute of Technology, it began operation in 1987 and was closed in 1992. The Naval Observatory later constructed a larger interferometer, the Navy Prototype Optical Interferometer.pp. 37–39, Overview of Multiple-Aperture Interferometry Binary Star Results from the Northern Hemisphere, Harold A. McAlister, pp.
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HD 217786 is a binary star about away. The primary main-sequence star belongs to the spectral class of F8. It is much older than Sun and is depleted of heavy elements, having 65% of solar abundance. The red dwarf stellar companion at a projected separation of 155 AU was discovered in 2016, and no other companion stars were detected at separations from 2.74 to 76.80 AUs.
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57 Cygni is a close binary star system in the constellation Cygnus, located about 530 light years from Earth. It is visible to the naked eye as a blue- white hued star with a baseline apparent visual magnitude of 4.80. The pair have a magnitude difference of 0.34. This system is moving closer to the Earth with a heliocentric radial velocity of −21 km/s.
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HD 85622 is a binary star system in the southern constellation of Vela. It is visible to the naked eye with an apparent visual magnitude of 4.58. The distance to HD 85622 can be estimated from its annual parallax shift of , yielding a value of 750 light years. It is moving further from the Earth with a heliocentric radial velocity of +8 km/s.
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4 Cygni is a binary star system in the northern constellation of Cygnus. It is a faintly visible to the naked eye with an apparent visual magnitude of 5.17. The distance to 4 Cygni, as determined from its annual parallax shift of , is about 560 light years. This is single-lined spectroscopic binary with an orbital period of 35 days and an eccentricity of 0.45.
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Omicron Aurigae, Latinized from ο Aurigae, is the Bayer designation for an astrometric binary star system in the northern constellation of Auriga. With an apparent visual magnitude of 5.47, it is faintly visible to the naked eye. Based upon an annual parallax shift of , it is approximately distant from Earth. The star is a member of the Ursa Major stream of co-moving stars.
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17 Aquarii, abbreviated 17 Aqr, is a spectroscopic binary star system in the constellation of Aquarius. 17 Aquarii is the Flamsteed designation. It appears to the naked eye as a faint sixth magnitude star, having a combined apparent visual magnitude of 5.99. The distance to 17 Aqr can be estimated from its annual parallax shift of , which yields a separation of around 660 light years.
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26 Aquilae (abbreviated 26 Aql) is a binary star system in the equatorial constellation of Aquila. 20 Aquilae is its Flamsteed designation though it also bears the Bayer designation f Aquilae. It has an apparent visual magnitude of 5.00, which means it is faintly visible to the naked eye. As the Earth orbits the Sun, this star system undergoes a parallax shift of 21.15 mas.
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51 Aquarii is a binary star system located around 410 light years away from the Sun in the equatorial constellation of Aquarius. 51 Aquarii is its Flamsteed designation. It is visible to the naked eye as a dim, yellow-white hued star with a combined apparent visual magnitude of 5.78. The system is moving further from the Earth with a heliocentric radial velocity of +6 km/s.
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7 Aquarii, abbreviated 7 Aqr, is a binary star system in the zodiac constellation of Aquarius. 7 Aquarii is the Flamsteed designation. It is visible to the naked eye with an apparent visual magnitude of 5.5; the brighter component is baseline magnitude 5.62 while the faint secondary is magnitude 11.4. As of 2002, the pair had an angular separation of along a position angle of 165°.
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26 Andromedae, abbreviated 26 And, is an astrometric binary star system in the constellation Andromeda. 26 Andromedae is the Flamsteed designation. It has a combined apparent visual magnitude of 6.10, which is near the lower limit of visibility to the naked eye. The distance to this system can be estimated from its annual parallax shift of , which yields a range of 610 light years.
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47 Ophiuchi (47 Oph) is a binary star in the constellation Serpens. The combined apparent magnitude of the system is 4.54. The system is located about 98.1 light-years, or 30.1 parsecs away, based on its parallax as measured by Hipparcos. 47 Ophiuchi is a spectroscopic binary: that is, the two stars move fast enough that periodic Doppler shifts in the stars' spectra can be detected.
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Xi Cancri (ξ Cancri, abbreviated Xi Cnc, ξ Cnc) is a spectroscopic binary star system in the zodiac constellation of Cancer. It is visible to the naked eye with an apparent visual magnitude of +5.15. Based upon parallax measurements obtained during the Hipparcos mission, it is roughly 370 light-years distant from the Sun. The two components are designated Xi Cancri A (formally named Nahn ) and B.
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Chi Aurigae (χ Aur, χ Aurigae) is the Bayer designation for a binary star in the northern constellation of Auriga. It is faintly visible to the naked eye with an apparent visual magnitude of 4.74. The annual parallax shift of this object is much smaller than the measurement error, making distance estimates by that means unreliable. The estimated distance to this star is approximately 3,000 light years.
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Burnham disagrees, and dons a space suit to investigate in spite of the dangerous radiation from a nearby binary star system. She finds the object to be covered in ancient carvings, and guarded by an armed Klingon. The Klingon attacks, and when she uses her suit to escape she accidentally kills him. Burnham later awakens aboard the Shenzhou being treated for acute radiation sickness.
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Delta3 Tauri (δ3 Tauri) is a binary star system in the zodiac constellation of Taurus. Based upon an annual parallax shift of 21.96 mas as seen from Earth, it is located roughly 149 light years distant from the Sun. It is visible to the naked eye with a combined apparent visual magnitude of +4.32. δ3 Tauri is separated from δ1 Tauri by 0.72° on the sky.
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Vampirella originally hailed from the planet Drakulon, a world where blood flowed like water and where the natives, called the Vampiri, shared traditionally vampiric characteristics. Drakulon orbited a binary star which caused continuous droughts throughout the year. Unfortunately for the Vampiri, these droughts have gradually dried up their blood supply; threatening them with extinction. Vampirella's journey begins when an American space shuttle crashes on Drakulon.
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This star system was catalogued in the 1862 Bonner Durchmusterung ("Bonn astrometric Survey") as BD +18°4794B. It later appeared in Pickering's 1908 Harvard Revised Photometry Catalogue as HR 8210. The designation "IK Pegasi" follows the expanded form of the variable star nomenclature introduced by Friedrich W. Argelander. Examination of the spectrographic features of this star showed the characteristic absorption line shift of a binary star system.
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The minimum stable star to circumbinary planet separation is about 2-4 times the binary star separation, or orbital period about 3-8 times the binary period. The innermost planets in all the Kepler circumbinary systems (e.g. Kepler-16b, Kepler-451b and such) have been found orbiting close to this radius. The planets have semi-major axes that lie between 1.09 and 1.46 times this critical radius.
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15 Eridani is a binary star system in the equatorial constellation of Eridanus. It is visible to the naked eye as a faint, orange-hued star with an apparent visual magnitude of 4.875. Based upon parallax measurements, the system is located around 260 light years away from the Sun. It is moving further from the Earth with a heliocentric radial velocity of 24 km/s.
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38 Geminorum is a binary star system in the northern zodiac constellation of Gemini. It has the Bayer designation e Geminorum, while 38 Geminorum is the Flamsteed designation. This system is visible to the naked eye as a faint, white-hued point of light with an apparent visual magnitude of 4.71. The primary component is a magnitude 4.75 star, while the secondary is magnitude 7.80.
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HAT-P-1b is an extrasolar planet orbiting the Sun-like star HAT-P-1, also known as ADS 16402 B. HAT-P-1 is the dimmer component of the ADS 16402 binary star system. It is located roughly 521 light years away from Earth in the constellation Lacerta. HAT-P-1b is among the least dense of any of the known extrasolar planets.
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HR 5110, also known as BH Canum Venaticorum, is a binary star system in the northern constellation of Canes Venatici. It is visible to the naked eye with an apparent visual magnitude of 4.91. Based upon an annual parallax shift of , it is located 149 light years away. The system is moving further from the Sun with a heliocentric radial velocity of 6.4 km/s.
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89 Herculis is a binary star system located about 4,700 light years away from the Sun in the northern constellation of Hercules. It is visible to the naked eye as a faint, fifth magnitude star. The system is moving closer to the Earth with a heliocentric radial velocity of −28.5 km/s. This is a spectroscopic binary with the pair surrounded by a dusty disc.
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Omega Andromedae (ω And, ω Andromedae) is the Bayer designation for a slowly co-rotating binary star system in the northern constellation of Andromeda. Parallax measurements made during the Hipparcos mission make this system to be approximately from Earth. Its apparent visual magnitude is +4.83, which makes it bright enough to be seen with the naked eye. The primary component has a stellar classification of F5 IVe.
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HD 73389 is a binary star system in the constellation Carina. It has the Bayer designation e2 Carinae; HD 73389 is the identifier from the Henry Draper Catalogue. This system is visible to the naked eye as a point of light with a combined apparent visual magnitude of +4.84. Based on parallax measurements, it is located at a distance of approximately 225 light years from the Sun.
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HR 3220 is a binary star system in the southern constellation of Carina. It has the Bayer designation B Carinae; HR 3220 is the designation from the Bright Star Catalogue. It has a yellow-white hue and is visible to the naked eye with an apparent visual magnitude of 4.75. Based upon parallax measurements, it is located at a distance of 59 light years from the Sun.
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V376 Carinae is a binary star system in the southern constellation of Carina. It has the Bayer designation b1 Carinae; V376 Carinae is the variable star designation. The system is visible to the naked eye as a faint point of light with a combined apparent magnitude of +4.69. The distance to this system from the Sun is approximately 650 light years based on parallax.
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HD 69863 is a binary star system in the southern constellation of Carina. It is visible to the naked eye as a dim point of light with a combined apparent visual magnitude of 5.16. The system is located at a distance of about255 light years from the Sun based on parallax. The dual nature of this system was announced in 1832 by German astronomer Carl Rümker.
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Mu Aquarii, Latinized from μ Aquarii, is the Bayer designation for a binary star system in the equatorial constellation of Aquarius. It is visible to the naked eye with a combined apparent visual magnitude of 4.7. Based upon parallax measurements, the distance to this system is about . Mu Aquarii is a spectroscopic binary with an orbital period of 1,566 days and an eccentricity of 0.23.
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W Corvi is an eclipsing binary star system in the constellation Corvus, ranging from apparent magnitude 11.16 to 12.5 over 9 hours. Its period has increased by 1/4 second over a century. It is an unusual system in that its two stars are very close to each other yet have different surface temperatures and hence thermal transfer is not taking place as expected.
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69 Herculis is a binary star system in the northern constellation Hercules. It has the Bayer designation e Herculis, while 69 Herculis is the Flamsteed designation. This object is visible to the naked eye as a faint, white-hued star with a combined apparent visual magnitude of 4.63. The distance to this system can be estimated from parallax measurements, which yields a range of 175 light years.
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AI Phe is an eclipsing binary star identified in 1972. Its long mutual eclipses and combination of spectroscopic and astrometric data allows precise measurement of the masses and radii of the stars which is viewed as a potential cross-check on stellar properties and distances independent on Ceiphid Variables and such techniques. The long eclipse events require space-based observations to avoid Solar interference.
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Circinus X-1 is an X-ray binary star system that includes a neutron star. Observation of Circinus X-1 in July 2007 revealed the presence of X-ray jets normally found in black hole systems; it is the first of the sort to be discovered that displays this similarity to black holes. Circinus X-1 may be among the youngest X-ray binaries observed.
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Theta Hydrae, Latinized from θ Hydrae, is a binary star system in the constellation Hydra. It is visible to the naked eye with an apparent visual magnitude of 3.9. The star system has a high proper motion with an annual parallax shift of , indicating a distance of about . Theta Hydrae forms a double with a magnitude 9.9 star located at an angular separation of .
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HD 81799 (G Hydrae) is a suspected astrometric binary star system in the equatorial constellation of Hydra. It is visible to the naked eye with an apparent visual magnitude of 4.69. The distance to this system, as determined from an annual parallax shift of , is 164 light years. It is moving further away from the Earth with a heliocentric radial velocity of 29 km/s.
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Phi3 Hydrae (φ3 Hya) is a binary star in the equatorial constellation of Hydra. It originally received the Flamsteed designation of 2 Crateris before being placed in the Hydra constellation. Based upon an annual parallax shift of 15.49 mas as seen from Earth, it is located around 211 light years from the Sun. It is visible to the naked eye with an apparent visual magnitude of 4.90.
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Chi1 Hydrae (χ1 Hydrae) is a binary star in the equatorial constellation of Hydra. It originally received the Flamsteed designation of 9 Crateris before being placed in the Hydra constellation. Based upon an annual parallax shift of 22.8 mas as seen from Earth, it is located about 143 light years from the Sun. It is visible to the naked with a combined apparent visual magnitude of 4.94.
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54 Leonis is a binary star system in the zodiac constellation of Leo, located around 321 light years from the Sun. It is visible to the naked eye as a faint, white-hued star with a combined apparent visual magnitude of 4.30. As of 2017, the pair had an angular separation of along a position angle of 113°. They have a physical separation of around .
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10 Vulpeculae is an astrometric binary star system in the northern constellation of Vulpecula. It is faintly visible to the naked eye with an apparent visual magnitude of 5.497. The system is located roughly 330 light years from the Sun, as determined from an annual parallax shift of . It is moving closer to the Sun with a heliocentric radial velocity of −9.9 km/s.
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V4641 Sagittarii (V4641 Sgr) is a variable X-ray binary star system in the constellation Sagittarius. It is the source of one of the fastest superluminal jets in the Milky Way galaxy. In 1999 a violent X-ray outburst revealed it to contain a black hole. At the time, it was considered to be the closest known black hole to Earth, at a distance of approximately .
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N Centauri is a binary star in the southern constellation of Centaurus. It is dimly visible to the naked eye with an apparent visual magnitude of 5.26. The distance to this system is approximately 311 light years based on parallax, and it has an absolute magnitude of +0.76. The system is drifting further away from the Sun with a radial velocity of +27 km/s.
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The nova system is thus a binary star, and a classical nova. V339 Del is the first nova that has been observed to synthesize the element lithium. Production of lithium-7 from the decay of beryllium-7, which was observed in the wind blown out of the nova. This is the first direct evidence of the supply of lithium to the interstellar medium by an astronomical object.
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35 Cygni is a spectroscopic binary star in the constellation Cygnus. Its apparent magnitude is 5.18. Located around distant, its primary is a yellow supergiant of spectral type F6Ib, a massive star that has used up its core hydrogen and is now fusing heavier elements. Yellow supergiants are usually variable, often Classical Cepheid variables, but 35 Cyg is notable for having an especially constant brightness.
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Its distance has been estimated anywhere from one to six kpc. The General Catalogue of Variable Stars classifies it as an Orion variable, a pre-main sequence star, but other authors consider it to be a supergiant B[e] star. It has been confirmed to be a binary star system with the two stars separated by about 52 AU, but the nature of the companion is unknown.
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Neel V. Patel, MIT Technology Review. 2 October 2019. Quote: surface conditions are dependent on a host of different individual properties of that planet, such as internal and geological processes, magnetic field evolution, climate, atmospheric escape, rotational effects, tidal forces, orbits, star formation and evolution, unusual conditions like binary star systems, and gravitational perturbations from passing bodies. This misunderstanding is reflected in excited reports of 'habitable planets'.
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Sigma2 Gruis is a binary star system in the southern constellation of Grus. Its apparent visual magnitude is 5.86. The pair had an angular separation of 2.7 arc seconds along a position angle of 265°, as of 1991. Located around distant, the white-hued primary component is an A-type main-sequence star of spectral type A1V, a star that is currently fusing its core hydrogen.
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Eta Persei (η Persei, abbreviated Eta Per, η Per), is a binary star and the 'A' component of a triple star system (the 'B' component is the star HD 237009) in the constellation of Perseus . It is approximately 1331 light-years away from Earth. The two components of Eta Persei itself are designated Eta Persei A (officially named Miram , a recent name for the system) and B.
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Gamma Centauri (γ Cen, γ Centauri) is a star in the southern constellation Centaurus. It has the proper name Muhlifain, not to be confused with Muliphein, which is γ Canis Majoris; both names derive from the same Arabic root. It is a binary star system about from Earth. The combined apparent visual magnitude of the pair is +2.17; individually they are third magnitude stars.
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On 2 September 1918 Ellison was appointed Director of the Armagh Observatory. He found the Observatory in a state of disrepair and set about repairing the instruments and the observatory dome. On 3 January 1919 he deeded a telescope of his own to the observatory, an 18 inch reflecting telescope, which is still there. Ellison was a highly regarded planetary and binary star observer.
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BD+20°307 is a close binary star system approximately 300 light-years away in the constellation Aries. The system is surrounded by a dusty ring. The dust that orbits around several hundred main-sequence stars is cold and comes from a Kuiper-belt analogous region. In the Solar System the ongoing collisions between asteroids generate a tenuous cloud of dust known as the zodiacal light.
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A visual binary is a gravitationally bound binary star system that can be resolved into two stars. These stars are estimated, via Kepler's 3rd law, to have periods ranging from a few years to thousands of years. A visual binary consists of two stars, usually of a different brightness. Because of this, the brighter star is called the primary and the fainter one is called the companion.
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This is a single-lined spectroscopic binary star system. The pair have a nearly circular orbit with an eccentricity of at or below 0.03 and a period of . The primary has an value of , which only gives a lower bound for the semimajor axis a since the orbital inclination i to the line of sight is unknown. The system is a source for X-ray emission.
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15 Lyncis is a binary star system in the northern constellation of Lynx. It is visible to the naked eye as a faint point of light with a combined apparent visual magnitude of 4.35. Based on the system's parallax, it is located 178 light-years (54.7 parsecs) away. The pair are moving away from the Earth with a heliocentric radial velocity of +2 km/s.
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32 Eridani is divisible in small amateur telescopes. 39 Eridani is a binary star also divisible in small amateur telescopes, 206 light-years from Earth. The primary is an orange-hued giant star of magnitude 4.9 and the secondary is of magnitude 8. 40 Eridani is a triple star system consisting of an orange main-sequence star, a white dwarf, and a red dwarf.
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43 Persei is a binary star Vizier catalog entry system in the northern constellation Perseus. It is visible to the naked eye as a dim, yellow-white hued star with an apparent visual magnitude of 5.28. The system is located around distant from the Sun, based on parallax. This is a double-lined spectroscopic binary with an orbital period of 30.4 days and an eccentricity of 0.6.
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Zeta Centauri, Latinized from ζ Centauri, is a binary star system in the southern constellation of Centaurus. It has the proper name Alnair , from the scientific-Arabic Nayyir Badan Qanṭūris (نير بطن قنطورس), meaning "The Bright (Star) of the Body of the Centaur".ibid., p.28. With a combined apparent visual magnitude of +2.55, it is one of the brighter members of the constellation.
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This was the SM4 mission. An example of astrometry science with the Hubble FGS system is observations of the Low-Mass Binary star system L722-22. Observations were taken of the system in 1990s, and the data helped determine the mass of each of the components of L722-22, which is also known as LHS 1047 and GJ 1005. The FGS are white-light shearing interferometers.
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For example, there is no known complete solution for a spacetime with two massive bodies in it (which is a theoretical model of a binary star system, for example). However, approximations are usually made in these cases. These are commonly referred to as post-Newtonian approximations. Even so, there are several cases where the field equations have been solved completely, and those are called exact solutions.
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Groombridge 34 is a binary star system in the northern constellation of Andromeda. It was listed as entry number 34 in A Catalogue of Circumpolar Stars, published posthumously in 1838 by British astronomer Stephen Groombridge. Based upon parallax measurements taken by the Gaia spacecraft, the system is located about 11.6 light-years from the Sun. This positions the pair among the nearest stars to the Solar System.
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Using direct focussing observations of the non-thermal source in the extremely hard X-ray band that is spatially coincident with the star, they showed that the source of non-thermal X-rays varies with the orbital phase of the binary star system and that the photon index of the emission is similar to that derived through analysis of the γ-ray (gamma) spectrum.
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HD 40409 is a suspected astrometric binary star system in the southern constellation of Dorado. It is a faint system but visible to the naked eye with an apparent visual magnitude of 4.65. Based upon an annual parallax shift of , it is located 88 light years away from the Sun. It is moving further away with a heliocentric radial velocity of +25 km/s.
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Tau9 Eridani (τ9 Eri) is a binary star in the constellation Eridanus. It is visible to the naked eye with an apparent visual magnitude of 4.63. The distance to this system can be estimated using the parallax method, which yields a value of roughly 327 light years. This is a single-lined spectroscopic binary system with an orbital period of 5.9537 days and an eccentricity of 0.1.
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13 Scorpii, also known by its Bayer designation c2 Scorpii, is a binary star in the constellation Scorpius. Its apparent magnitude is 4.57, meaning it can be faintly seen with the naked eye. Based on parallax estimates made by the Hipparcos spacecraft, the system is located about 480 light-years (147 parsecs) away. It is located within the Upper Scorpius subgroup of the Scorpius–Centaurus Association.
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HD 175535 is a binary star system in the northern circumpolar constellation of Draco. It has an apparent visual magnitude of 4.92, which is bright enough to be faintly visible to the naked eye. The system is located about 302 light years away, as determined from its annual parallax shift of . It is moving further from the Earth with a heliocentric radial velocity of +8.5 km/s.
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Gamma Canis Minoris (γ Canis Minoris) is a binary star system in the equatorial constellation Canis Minor. Its orange colour is obvious when seen through binoculars. The system is visible to the naked eye with a combined apparent visual magnitude of +4.33. Based upon an annual parallax shift of 10.25 mas as seen from Earth, this system is located about 320 light years from the Sun.
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Xi2 Canis Majoris, which is Latinized from ξ2 Canis Majoris, is an astrometric binary star system in the southern constellation of Canis Major. With an apparent visual magnitude of +4.54, it is visible to the naked eye. Based upon an annual parallax shift of , the system is approximately 390 light years distant from Earth. It is receding with a radial velocity of +26 km/s.
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Omega Eridani (ω Eri) is a binary star system in the constellation Eridanus. It is visible to the naked eye with an apparent visual magnitude is 4.37. The distance to this star, as determined by the parallax method, is around 235 light years. This is a single-lined spectroscopic binary system with an orbital period of 3,057 days (8.4 years) and an eccentricity of 0.46.
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This star is considered a solar analog—meaning that it is photometrically analogous to the Sun. Like the Sun, it has a magnetic activity cycle. It shares a common proper motion through space with the spectroscopic binary star system HD 122742, and in the past the three may have formed a triple star system. In the Bright Star Catalogue, it was noted as having an infrared excess.
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13 Comae Berenices is a probable binary star system in the northern constellation of Coma Berenices. It has an apparent visual magnitude of 5.17, which is bright enough to be faintly visible to the naked eye. With an annual parallax shift of 12.33 mas, it is located around 260 light years from the Sun. It is member of the nearby Coma Star Cluster (Melotte 111).
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BY Draconis is a multiple star system in the constellation Draco, consisting of at least three components. Components A and B are main sequence stars, and form a close binary star system with a short orbital period of only 5.98 days. Their individual spectroscopic classifications are dK5e and dK7e. They form the prototype of a class of variable stars known as BY Draconis variables.
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Xi Aquarii (ξ Aquarii, abbreviated Xi Aqr, ξ Aqr) is a binary star system in the equatorial constellation of Aquarius. It is visible to the naked eye with an apparent visual magnitude of 4.7. Based upon parallax measurements made during the Hipparcos mission, this system lies at a distance of around from the Sun. The two components are designated Xi Aquarii A (also named Bunda) and B.
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17 Leporis is a binary star system in the southern constellation of Lepus.§1, Verhoelst, van Aarle, and Acke, 2007. It has an overall apparent visual magnitude which varies between 4.82 and 5.06, making it luminous enough to be visible to the naked eye as a faint star. The variable star designation for this system is SS Leporis, while 17 Leporis is the Flamsteed designation.
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Eta Horologii (η Horologii, η Hor) is a binary star system in the southern constellation of Horologium. It is visible to the naked eye with a combined apparent visual magnitude of 5.31. Based upon an annual parallax shift of 21.95 mas as seen from Earth, it is located around 149 light years from the Sun. The orbit for this pair is not yet well constrained.
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The Star Kingdom of Manticore is the star nation that occupies the Manticore binary star system. It is a monarchy and the current ruler is Queen Elizabeth III of the House of Winton. The binary Manticore System was located 512 light-years to the Galactic north of the Sol System and Earth. It contained three habitable planets: Gryphon, Sphinx, and the capital planet Manticore.
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Theta1 Crucis (θ1 Cru, Theta1 Crucis) is a spectroscopic binary star system in the southern constellation of Crux. It is visible to the naked eye with an apparent visual magnitude of 4.30m. The distance to this star, as determined using parallax measurements, is around 235 light years. The pair orbit each other closely with a period of 24.5 days and an eccentricity of 0.61.
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Xi Piscium (ξ Piscium) is an orange-hued binary star system in the zodiac constellation of Pisces. In 1690, the astronomer Johannes Hevelius in his Firmamentum Sobiescianum regarded the constellation Pisces as being composed of four subdivisions. Xi Piscium was considered to be part of the Linum Austrinum, the South Cord. The star is visible to the naked eye, having an apparent visual magnitude of 4.60.
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DD Microscopii, also known as CD-43 14304, is a binary star system in the constellation Microscopium. Its apparent magnitude is 11.0.SIMBAD, DD Microscopii (accessed 25 March 2015) It is a symbiotic star system composed of an orange giant of spectral type K2III and white dwarf in close orbit, with the smaller star ionizing the stellar wind of the larger star. The system is metal-poor.
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HD 133131 is a binary star in the constellation of Libra. It is roughly 168 light-years (51.5 parsecs) away from the Sun. It consists of two G-type main- sequence stars; neither are bright enough to be seen with the naked eye. Both components, HD 133131 A and B, are very similar to the Sun but are far older, about 6 billion years old.
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Rho Leonis (ρ Leo) is a binary star in the zodiac constellation of Leo, and, like the prominent nearby star Regulus, is near the ecliptic. With an apparent visual magnitude of 3.9, this star can be readily seen with the naked eye. Parallax measurements give a distance estimate of about from the Earth. This is an enormous star with about 21 times the Sun's mass () and 37 times the Sun's radius.
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20 Persei is a visual binary star in the northern constellation of Perseus, a few degrees from Pi Persei. It is visible to the naked eye as a dim, yellow- white hued point of light with a combined apparent visual magnitude of 5.343. The system is located around away from the Sun, based on its parallax. It is receding from the Earth with a heliocentric radial velocity of +6 km/s.
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Phi Virginis (φ Virginis, abbreviated Phi Vir, φ Vir) is a binary star in the zodiac constellation of Virgo. It can be seen with the naked eye, having an apparent visual magnitude of +4.81. Based upon parallax measurements obtained during the Hipparcos mission, it is located roughly distant from the Sun. The two components are designated Phi Virginis A (officially named Elgafar , the traditional name for the system) and B.
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Nu2 Sagittarii (ν2 Sagittarii) is a binary star system in the zodiac constellation of Sagittarius. It is faintly visible to the naked eye, having an apparent visual magnitude of +4.98. Based upon a small annual parallax shift of 11.91 mas as seen from Earth, this system is located around 270 light years from the Sun. Nu2 Sagittarii has a high peculiar velocity of and is most likely a runaway star system.
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The rotation period of the star, 6.3 days, is known from the light curve obtained by the Kepler spacecraft, causing periodic variations of about 2% in the brightness of the star as star spots appear and disappear from Earth's line of sight. This stellar variability was removed for the analysis of the transit signal of the planet K2-33b. K2-33 is almost certainly not a binary star.
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Beta Serpentis, Latinized from β Serpentis, is a binary star system in the constellation Serpens, in its head (Serpens Caput). It is visible to the naked eye with a combined apparent visual magnitude of +3.65. Based upon an annual parallax shift of 21.03 mas as seen from Earth, it is located around 155 light years from the Sun. The system is a member of the Ursa Major Moving Group.
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70 Pegasi is a binary star system in the northern constellation Pegasus. It is a faint star, visible to the naked eye under good seeing conditions, with an apparent visual magnitude of 4.56. The measured annual parallax shift measured from Earth's orbit is 18.65 mas, yielding a distance estimate of around 175 light years. The visual magnitude of the star is diminished by an extinction of due to interstellar dust.
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Theta Ursae Minoris, Latinized from θ Ursae Minoris, is a suspected binary star system that is visible to the naked eye in the northern circumpolar constellation of Ursa Minor. It is roughly 860 light years from Earth with an apparent visual magnitude of 5.0. The system is moving closer to the Sun with a radial velocity of −25 km/s. This is a probable spectroscopic binary with two roughly equal components.
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Its Arabic name comes from the phrase mankib dhu al-'inan, meaning "shoulder of the charioteer" and is a reference to Beta Aurigae's location in the constellation. Menkalinan is 81 light-years away and has a magnitude of 1.90. Like Epsilon Aurigae, it is an eclipsing binary star that varies in magnitude by 0.1m. The two components are blue-white stars that have a period of 3.96 days.
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Auriga is home to several less prominent binary and double stars. Theta Aurigae (Bogardus, Mahasim) is a blue-white A0p class binary star of magnitude 2.62 with a luminosity of . It has an absolute magnitude of 0.1 and is 165 light- years from Earth. The secondary is a yellow star of magnitude 7.1, which requires a telescope of in aperture to resolve; the two stars are separated by 3.6 arcseconds.
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ADS 16402 is a binary star system, composed of two sun-like stars located approximately 525 light-years away in the constellation Lacerta. It was first identified by John Herschel in 1831. The two stars are separated by 11.26 arcseconds which leads to a projected separation of roughly 1500 astronomical units at the distance of ADS 16402. The star system is estimated to be 1.9 ± 0.6 billion years old.
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4 Aquarii (abbreviated 4 Aqr) is a binary star system in the constellation Aquarius, located approximately 198 light years away from the Sun. 4 Aquarii is the Flamsteed designation. It is visible to the naked eye as a dim, yellow- white hued star with a combined apparent visual magnitude of 5.99. The system is moving closer to the Earth with a heliocentric radial velocity of −21.5 km/s.
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Lambda Columbae, Latinized from λ Columbae, is a probable binary star in the southern constellation of Columba. With an apparent visual magnitude of 4.86, it is faintly visible to the naked eye. The measured annual parallax shift of 9.75 mas yields an estimated distance of roughly 335 light years. Lambda Columbae has a stellar classification of B5 V, indicating that it is a B-type main sequence star.
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The secondary is of magnitude 4.0 and has a modest separation, appearing only under intense magnification due to its distance. The northerly star Theta Centauri, officially named Menkent, is an orange giant star of magnitude 2.06. It is the only bright star of Centaurus that is easily visible from mid-northern latitudes. The next bright object is Gamma Centauri, a binary star which appears to the naked eye at magnitude 2.2.
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Q Centauri (Q Cen) is a binary star in the constellation Centaurus. It has a combined apparent magnitude of +4.99 and is approximately 270 light years from Earth. The primary component, Q Centauri A, is a blue-white B-type main sequence dwarf with an apparent magnitude of +5.7. Its companion, Q Centauri B, is a white A-type main sequence dwarf with an apparent magnitude of +7.1.
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Alpha Fornacis (α Fornacis, abbreviated Alpha For, α For) is a binary star system in the southern constellation of Fornax. It is the brightest star in the constellation and the only one brighter than magnitude 4.0. Based on parallax measurements obtained during the Hipparcos mission, it is approximately 46 light-years (14 parsecs) distant from the Sun. Its two components are designated Alpha Fornacis A (officially named Dalim ) and B.
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Tau Ursae Majoris (τ UMa) is the Bayer designation for a binary star in the northern circumpolar constellation of Ursa Major. It is visible to the naked eye, having an apparent visual magnitude of 4.66. With an annual parallax shift of 25.82 mas, it is located about 126 light years from the Sun. At that distance, the visual magnitude is diminished by an extinction factor of 0.19 due to interstellar dust.
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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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HD 41534 is a binary star system in the southern constellation of Columba. It is dimply visible to the naked eye with a combined apparent visual magnitude of 5.65. The distance to this system is approximately 950 light-years based on parallax, and it is receding from the Sun with a radial velocity of +93 km/s. This is a runaway star system with an unusually high peculiar velocity of .
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Beta Arietis has an apparent visual magnitude of 2.66. Based on parallax measurements, it is located at a distance of from Earth. This is a spectroscopic binary star system consisting of a pair of stars orbiting around each other with a separation that can not currently be resolved with a conventional telescope. However, the pair have been resolved using the Mark III Stellar Interferometer at the Mount Wilson Observatory.
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HD 202951 is a probable binary star system located in the northern constellation of Equuleus. It is near the lower limit of visibility to the naked eye, having an apparent visual magnitude of 5.97. The distance to this system can be estimated from the annual parallax shift of , yielding a value of roughly 1,190 light years. It is moving closer with a heliocentric radial velocity of −37 km/s.
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NGC 6326 is a complex and irregularly structured planetary nebula located in the constellation Ara. It was discovered by Scottish astronomer James Dunlop on 26 August 1826. NGC 6326 is the result of the ejected material from the central binary star, which is nearing the end of its life. The blue and red color is due to the amount of radiation the star releases, thus causing the gasses to glow.
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Delta Delphini, Latinized from δ Delphini, is a binary star in the northern constellation of Delphinus. It is visible to the naked eye with an apparent visual magnitude of 4.43. Based upon an annual parallax shift of 14.61 mas as seen from the Earth, the system is located about 223 light years from the Sun. This is a double-lined spectroscopic binary system with an orbital period of 40.58 days.
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EQ Pegasi was first noticed to be a binary star by Carl A. Wirtanen who in the course of a systematic survey of the McCormick Observatory photographic plates for M-type dwarfs, detected a companion about two magnitudes fainter at a separation of 3.5 arcseconds. Both components are also though to be single- lined spectroscopic binaries, with faint companions that have not been resolved in orbits of a few years.
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HD 104304 (24 G. Virginis) is a binary star in the zodiac constellation Virgo. It has an apparent magnitude of 5.54, making it visible to the unaided eye under suitable viewing conditions. The stellar classification of G8 IV means that this is a subgiant star that has left the main sequence and has begun to evolve into a giant star. In 2007, a candidate planet was announced orbiting this star.
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Phi Cygni, Latinized from φ Cygni, is a binary star system in the northern constellation of Cygnus. It is faintly visible to the naked eye with an apparent visual magnitude of 4.70. The annual parallax shift is 12.25 mas as measured from Earth, which yields a distance estimate of around 266 light years. It is moving further from the Sun with a radial velocity of +4.5 km/s.
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This is a single-lined spectroscopic binary star system with an orbital period of 258.48 days and an eccentricity of 0.21. The primary, component A, is an evolved K-type giant star with a stellar classification of K0 III. It is a suspected barium star, which may indicate the orbiting companion, component B, is a white dwarf star. The measured angular diameter of the primary, after correction for limb darkening, is .
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U Aquilae is a binary star system in the constellation Aquila, Located approximately away from Earth. The primary star (component A) is a yellow supergiant with a radius of and a luminosity of . The secondary (component B) is a blue main-sequence star, twice the mass of the sun and around thirty times more luminous. It is hotter than the primary star at 9,300 K, but much smaller and fainter.
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16 Vulpeculae is a binary star system in the northern constellation Vulpecula. It has a combined apparent visual magnitude of 5.787, which is near the lower limit of visibility to the naked eye. Based upon an annual parallax shift of as seen from Earth's orbit, it is located about 222 light years away. The system is moving closer to the Sun with a heliocentric radial velocity of about −37 km/s.
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41 Aurigae is a binary star system located around 310–316 light years away from the Sun in the northern constellation of Auriga. It is visible to the naked eye as a dim, white-hued star with a combined apparent visual magnitude of 5.83. This system is moving further from the Earth with a heliocentric radial velocity of 31 km/s. It is a probable member of the Hyades Supercluster.
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Nebula IC 405 around AE Aurigae AE Aurigae is a blue O-type main sequence dwarf with a mean apparent magnitude of +6.0. It is classified as an Orion type variable star and its brightness varies irregularly between magnitudes +5.78 and +6.08. It is approximately 1,300 light-years from Earth. AE Aur is a runaway star that might have been ejected during a collision of two binary star groups.
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7 Arietis (abbreviated 7 Ari) is a binary star system in the northern constellation of Aries. 7 Arietis is the Flamsteed designation. The pair have a combined apparent visual magnitude of 5.76, making it faintly visible to the naked eye from dark suburban skies. Based upon an annual parallax shift of 5.85 mas, it is approximately distant from the Earth, give or take a 40 light- year margin of error.
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23 Aquilae is a binary star system in the equatorial constellation of Aquila. 23 Aquilae is its Flamsteed designation. It is at a distance of about with an apparent visual magnitude of 5.10, which is bright enough to be faintly visible to the naked eye as an orange-hued star. The brightness of the star is diminished by 0.21 in magnitude because of extinction from interstellar dust and gas.
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Nu2 Boötis is a white-hued binary star system in the northern constellation of Boötes. It is faintly visible to the naked eye with a combined apparent visual magnitude of 5.02. Based upon an annual parallax shift of 7.86 mas as seen from the Earth, it is located roughly 415 light years from the Sun. The system is moving closer to the Sun with a radial velocity of −16.6 km/s.
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83 Aquarii (abbreviated 83 Aqr) is a binary star system in the equatorial constellation of Aquarius. 83 Aquarii is its Flamsteed designation, though it also bears the Bayer designation of h Aquarii. The combined apparent visual magnitude of the pair is 5.43, which is faintly visible to the naked eye. Based upon an annual parallax shift of 15.57 milliarcseconds, it is located at a distance of around from Earth.
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32 Aquarii is a binary star system in the zodiac constellation of Aquarius. 32 Aquarii is its Flamsteed designation. It is visible to the naked eye as a dim, white-hued star with an apparent visual magnitude of 5.29. This system is moving away from the Earth with a heliocentric radial velocity of +19 km/s, and is a possible member of the corona of the Ursa Major flow.
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Zeta Cygni (ζ Cyg) is a binary star system in the northern constellation of Cygnus, the swan. It has an apparent visual magnitude of 3.26 and, based upon parallax measurements, is about away. The primary component, ζ Cyg A is a giant star with a spectral type of G8 IIIp. Its most likely status is as a red clump giant, an evolved star that has begun core helium fusion.
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1 Boötis (1 Boo) is a binary star system in the northern constellation of Boötes, located 318 light years away from the Sun. It is visible to the naked eye as a dim, white-hued star with a combined apparent visual magnitude of 5.71. The pair had an angular separation of as of 2008. It is moving closer to the Earth with a heliocentric radial velocity of −26 km/s.
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Lambda Cancri (λ Cancri, abbreviated Lambda Cnc, λ Cnc) is a blue-white hued spectroscopic binary star in the zodiac constellation of Cancer. With a combined apparent visual magnitude of +5.93, it is faintly visible to the naked eye. Based upon parallax measurements obtained during the Gaia mission, it is about 550 light-years distant from the Sun. The two components are designated Lambda Cancri A (formally named Piautos ) and B.
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20 Leonis Minoris is a binary star system in the northern constellation of Leo Minor. It is faintly visible to the naked eye, having an apparent visual magnitude of +5.4. Based upon an annual parallax shift of 66.46 mas, it is located 49 light years from the Sun. The star has a relatively high proper motion and is moving away from the Sun with a radial velocity of +56 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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Psi Centauri, which is Latinized from ψ Centauri, is a binary star system in the southern constellation of Centaurus. It is visible to the naked eye with a baseline apparent visual magnitude of +4.05. The distance to this system is approximately 259 light years based on parallax. The radial velocity is poorly constrained, but it appears to be slowly drifting away from the Sun at the rate of +2 km/s.
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Omicron1 Orionis (ο1 Ori) is a binary star in the northeastern corner of the constellation Orion. It is visible to the naked eye with an apparent visual magnitude of 4.7. Based upon an annual parallax shift of , it is located approximately 650 light years from the Sun. At that distance, the visual magnitude of the star is diminished by an interstellar absorption factor of 0.27 due to intervening dust.
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The planet orbits in a circumbinary orbit around a (G-type) and (M-type) binary star system. The stars orbit each other about every 7.45 days. The stars have masses of 1.04 and 0.35 and radii of 0.96 and 0.35 , respectively. They have temperatures of 5636 K and 3357 K. Based on the stellar characteristics, an estimated age of 4–5 billion years for the system is possible.
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Delta2 Telescopii is a blue-white hued binary star system in the southern constellation of Telescopium. It is faintly visible to the naked eye, having an apparent visual magnitude of 5.05. The distance to this system, as determined with an annual parallax shift of 2.73 mas, is roughly 1,200 light years. At that distance, the visual magnitude of the star is diminished by an extinction of 0.36 due to interstellar dust.
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Artist's conception of two heartbeat stars and a companion star. (NASA/JPL- Caltech) Heartbeat stars are pulsating variable binary star systems with vibrations caused by tidal forces. The name "heartbeat" comes from the similarity of the light curve of the star with what a heartbeat looks like through an electrocardiogram if their brightness was mapped over time. Many heartbeat stars have been discovered with the Kepler Space Telescope.
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Phi Geminorum, Latinized from φ Geminorum, is a binary star in the constellation Gemini, to the southwest of Pollux. It is visible to the naked eye with an apparent visual magnitude of 4.95. Based upon an annual parallax shift of 14.66 mas, this system is located around 220 light years from the Sun. The two components of this system have a circular orbit with a period of 582 days.
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Kepler-47 is a binary star system with three exoplanets in orbit around the pair of stars located about 1055 parsecs (3,442 light years) away from Earth. The first two planets announced are designated Kepler-47b, and Kepler-47c. Kepler-47 is the first circumbinary multi-planet system discovered by the Kepler mission. The outermost of the planets is a gas giant orbiting within the habitable zone of the stars.
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Mu2 Octantis (μ2 Oct) is a binary star system of two G-type main-sequence stars. It shares the designation μ with μ1 Octantis, from which it is separated by 50 arcminutes. The primary star (A) is HD 196067, whose data is in the starbox. The secondary star (B) is HD 196068 (HIP 102128, LTT 8160), another G-type main-sequence star with an apparent magnitude of 7.18.
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This star lies about 5° from the galactic plane and about 30° from the line of sight to the Galactic Center. This region of the sky is crowded with other objects along the line of sight, with at least 55 located within 10 arcseconds of the star. Examination of the star shows no companions with an 85% probability. Despite this, it is suspected of being a spectroscopic binary star.
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Phi Aquilae, Latinized from φ Aquilae, is the Bayer designation of a binary star system in the equatorial constellation of Aquila. It has an apparent visual magnitude of +5.28 and is visible to the naked eye. With an annual parallax shift of 14.86 mas, this star is located at a distance of approximately from Earth. Phi Aquilae is a single-lined spectroscopic binary with an orbital period of 3.32068 days.
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Eta Andromedae (Eta And, η Andromedae, η And) is a spectroscopic binary star in the constellation of Andromeda. It consists of two G-type subgiant or giant stars orbiting each other with a period of 115.7 days and has an overall apparent visual magnitude of approximately 4.403.The spectroscopic binary eta Andromedae: Determination of the orbit by optical interferometry, C. A. Hummel et al., Astronomical Journal 106, #6 (December 1993), pp.
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Mu1 Gruis, Latinized from μ1 Gruis, is a binary star system in the southern constellation of Grus. It is visible to the naked eye with a combined apparent visual magnitude of 4.79. The distance to this system, as determined using an annual parallax shift of 11.44 mas as seen from the Earth, is around 275 light years. It is drifting closer with a heliocentric radial velocity of −5 km/s.
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Gliese 3685 is a star in the constellation of Leo. It is extremely faint; its apparent magnitude is 13.3, and can only be seen with a ten-inch (25 cm) telescope (see Limiting magnitude). Based on a parallax of 50.30 milliarcseconds, the system is located 65 light years (20 parsecs) away from the Earth. This is a part of a binary star system consisting of two components separated by 24″.
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Eggleton and Tokovinin (2008) listed this as a suspected binary star system consisting of two roughly equal components. It appears as an ageing red giant with a stellar classification of M0III. This is a suspected semiregular variable star with a very small amplitude and a period of 40 days or more. Having exhausted the supply of hydrogen at its core, it has expanded to 44 times the Sun's radius.
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The planet orbits in a circumbinary orbit around a (G-type) and (M-type) binary star system. The stars orbit each other about every 7.45 days. The stars have masses of 1.04 and 0.35 and radii of 0.96 and 0.35 , respectively. They have temperatures of 5636 K and 3357 K. Based on the stellar characteristics and orbital dynamics, an estimated age of 4–5 billion years for the system is possible.
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30 Herculis is a binary star system in the northern constellation of Hercules. It has the Bayer designation g Herculis, while 30 Herculis is the Flamsteed designation. This system is visible to the naked eye as a faint, red-hued point of light with a baseline apparent visual magnitude of 4.83. Based upon a measured parallax of , it is located around 354 light years away from the Sun.
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II Pegasi is a binary star system in the constellation of Pegasus with an apparent magnitude of 7.4 and a distance of 130 light years. It is a very active RS Canum Venaticorum variable (RS CVn), a close binary system with active starspots. The primary (II Pegasi A) is a cool subgiant, an orange K-type star. It has begun to evolve off the main sequence and expand.
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He worked with the astrophysics staff, measuring the radial velocity of stars and determining the orbits of spectroscopic binaries. (The latter are binary star systems that could not be resolved with a telescope, but their orbital motions could be studied due to the doppler effect on their spectrum.) He was awarded his master's degree in 1907 from the University of Toronto. In 1909 he was married to Maude Eugenia Hall.
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Furthermore, all the distant stars, and much of interstellar space or intergalactic space is also likely filled with plasma, albeit at very low densities. Astrophysical plasmas are also observed in Accretion disks around stars or compact objects like white dwarfs, neutron stars, or black holes in close binary star systems.Mészáros, Péter (2010) The High Energy Universe: Ultra-High Energy Events in Astrophysics and Cosmology, Publisher: Cambridge University Press, , p. 99 .
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Delta Horologii (δ Horologii) is a binary star system in the constellation Horologium. It is visible to the naked eye with a combined apparent visual magnitude of 4.93. As of 2014, the pair had an angular separation of 0.20 arc seconds along a position angle of 24°. Based upon an annual parallax shift of 18.24 mas as seen from Earth, it is located 179 ± 4 light years from the Sun.
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Rho Hydrae, equally written ρ Hydrae, is a binary star in the equatorial constellation of Hydra. It is visible to the naked eye with an apparent visual magnitude of 4.34. The distance to this system, based upon an annual parallax shift of 9.21 mas, is about 354 light years. At that distance, the visual magnitude is diminished by an interstellar extinction of 0.06 magnitudes, due to intervening dust.
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Teal'c is a Jaffa from the planet Chulak, a planet orbiting a binary star system. Jaffa have a human appearance but have an abdominal pouch which serves as an incubator for a larval Goa'uld. The larval symbiote grants enhanced strength, health, healing, and longevity. Teal'c states he is 101 years old in season 4's "The Light", and ages an additional 50 years in season 10's "Unending".
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Stars in such close proximity will experience a high rate of interactions that can create binary star systems, as well as a type of star called a blue straggler that is formed by mass transfer. A process of mass segregation may have caused the central region to gain a greater proportion of higher mass stars, creating a color gradient with increasing blueness toward the middle of the cluster.
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Omicron Herculis is an eruptive variable of the Gamma Cassiopeiae class, which are rapidly rotating B-class stars with mass outflow. It has a projected rotational velocity of 194 km/s. Omicron Herculis is both a spectroscopic and an interferometric binary star with a separation of 0.1 arcsec. Omicron Hercules is notable for residing close to the coordinates of the solar apex, the direction towards which the Sun is moving.
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HR 4458 is a binary star system in the equatorial constellation of Hydra. It has the Gould designation 289 G. Hydrae; HR 4458 is the Bright Star Catalogue designation. At a distance of 31.13 light years, it is the closest star system to the solar system within this constellation. This object is visible to the naked eye as a dim, orange-hued star with an apparent visual magnitude of 5.97.
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A binary star system consists of two stars that orbit around their common centre of mass. The movements of both stars lie on a common orbital plane in space. When this plane is very closely aligned with the location of an observer, the stars can be seen to pass in front of each other. The result is a type of extrinsic variable star system called an eclipsing binary.
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The maximum luminosity of an eclipsing binary system is equal to the sum of the luminosity contributions from the individual stars. When one star passes in front of the other, the luminosity of the system is seen to decrease. The luminosity returns to normal once the two stars are no longer in alignment. The first eclipsing binary star system to be discovered was Algol, a star system in the constellation Perseus.
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Psi2 Orionis a binary star system in the equatorial constellation of Orion. It has an apparent visual magnitude of 4.60, indicating that it is visible to the naked eye. Based upon an annual parallax shift of 2.87 mass, it is roughly 1,100 light years distant from the Sun. This is a double-lined spectroscopic binary, which means that the individual absorption lines of both components can be discerned.
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Light curve for the Mira variable S Coronae Borealis over six years S Coronae Borealis (S CrB) is a Mira variable star in the constellation Corona Borealis. Its apparent magnitude varies between 5.8 and 14.1, with a period of 360 days—just under a year. Within the constellation, it lies to the west of Theta Coronae Borealis, and around 1 degree southeast of the eclipsing binary star U Coronae Borealis.
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A 2008 study concluded that the GSC 06200-00648 system (among others) is a binary star system allowing even more accurate determination of stellar and planetary parameters. TrES-4 orbits its primary star every 3.543 days and eclipses it when viewed from Earth. The study in 2012, utilizing a Rossiter–McLaughlin effect, have determined the planetary orbit is probably aligned with the equatorial plane of the star, misalignment equal to 6.3°.
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Binary stars are classified into four types according to the way in which they are observed: visually, by observation; spectroscopically, by periodic changes in spectral lines; photometrically, by changes in brightness caused by an eclipse; or astrometrically, by measuring a deviation in a star's position caused by an unseen companion. Any binary star can belong to several of these classes; for example, several spectroscopic binaries are also eclipsing binaries.
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The Captain and Humvee feel betrayed, but untie her. Searching the ship's database, the Captain and the Professor (Grant Swanby), who uses a wheelchair, discover that the legendary vampire hunter Abraham Van Helsing was one of the Captain's ancestors. The Professor believes Orlock will seek revenge against the Captain. The Captain learns how vampires can be stopped and decides to steer the Demeter on a course towards a binary star system.
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Omicron Piscium (ο Piscium, abbreviated Omi Psc, ο Psc) is a binary star in the constellation of Pisces. It is visible to the naked eye, having an apparent visual magnitude of 4.27. Based upon an annual parallax shift of 11.67 mas as seen from the Earth, the system is located roughly 280 light- years from the Sun. It is positioned near the ecliptic, so is subject to occultation by the Moon.
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XO-2Nb (or rarely XO-2Bb) is an extrasolar planet orbiting the star XO-2N, the fainter component of XO-2 wide binary star in the constellation Lynx. This planet was found by transit method in 2007 by Burke et al. This was the second such planet found by the XO telescope. The radial velocity of XO-2 over time, caused by the presence of XO-2 b.
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Phi Phoenicis, Latinized from φ Phoenicis, is a binary star system in the southern constellation of Phoenix. It is faintly visible to the naked eye with an apparent visual magnitude of 5.1. Based upon an annual parallax shift of 10.48 mas as seen from Earth, it is located around 310 light years from the Sun. It is moving away from the Sun with a radial velocity of 10.4 km/s.
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Sigma Librae (σ Librae, abbreviated Sigma Lib, σ Lib) is a binary star in the constellation of Libra. The apparent visual magnitude is +3.29, making it visible to the naked eye. Based upon parallax measurements, this system is at a distance of roughly from the Sun, with a 2% margin of error. At that distance, the visual magnitude is diminished by 0.20 ± 0.17 from extinction caused by intervening gas and dust.
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Tau2 Lupi, Latinized from τ2 Lup, is a binary star system in the constellation Lupus. It is visible to the naked eye with a combined apparent visual magnitude of 4.34. Based upon an annual parallax shift of 10.22 mas as seen from Earth, it is located around 319 light years from the Sun. The two components orbit each other with a period of 26.2 years and a high eccentricity of 0.94.
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It will produce a type Ib or Ic supernova within the next few hundred thousand years. WR 102c is surrounded by a shell of nebulosity which contains dust made even hotter than the star itself by intense radiation. The nebula also includes nearly of molecular hydrogen and around of ionised hydrogen, all expelled from the star. There is a suggestion that WR 102c may be a binary star.
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42 Persei is a binary star system in the northern constellation of Perseus. It has the Bayer designation n Persei, while 42 Persei is the Flamsteed designation. The system is visible to the naked eye as a dim, white-hued point of light with an apparent visual magnitude of 5.11. It is located around distant from the Sun, but is drifting closer with a radial velocity of −12.4 km/s.
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Spica is a close binary star whose components orbit each other every four days. They stay close together enough that they cannot be resolved as two stars through a telescope. The changes in the orbital motion of this pair results in a Doppler shift in the absorption lines of their respective spectra, making them a double-lined spectroscopic binary. Initially, the orbital parameters for this system were inferred using spectroscopic measurements.
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HD 114837 is a suspected binary star system in the southern constellation of Centaurus. The brighter star is faintly visible to the naked eye with an apparent visual magnitude of 4.90. It has a magnitude 10.2 candidate common proper motion companion at an angular separation of , as of 2014. The distance to this system, based on an annual parallax shift of as seen from Earth's orbit, is 59.3 light years.
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However, the star seems to be at most 20 million years old, which implies that it is a blue straggler, a star born from the merger of a binary star system, which was earlier ejected from the center of the Milky Way. In order for this to happen, there must have originally been a three-star system, or else there were two black holes and just the two stars.
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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 companion, a magnitude-7.6 star, is visible in binoculars and small amateur telescopes. η Gem (Propus) is a binary star with a variable component. 380 light-years away, it has a period of 500 years and is only divisible in large amateur telescopes. The primary is a semi-regular red giant with a period of 233 days; its minimum magnitude is 3.9 and its maximum magnitude is 3.1.
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Tau4 Eridani (τ4 Eridani, τ4 Eri) is a binary star system in the constellation Eridanus. It is visible to the naked eye with an apparent visual magnitude of 3.65. The distance to this star can be estimated using the parallax method, which yields a value of roughly 300 light years. This is an evolved red giant star currently on the asymptotic giant branch with a stellar classification of M3/4 III.
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HD 165189 and HD 165190 are components of a visual binary star system located 145 light years away in the southern constellation of Corona Australis. It is visible to the naked eye with the primary having an apparent visual magnitude of . The system is a member of the Beta Pictoris Moving Group. The pair orbit each other with a period of 450 years and a large eccentricity of 0.650.
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This is a binary star system with an orbital period of 52.1 days and an eccentricity of 0.22. Only the primary star can be directly detected, via Doppler shifts or perturbations around the system's barycenter. Using spectroscopy and astrometry, the nature of the secondary star can be inferred. The primary star is an F-type main-sequence star with a stellar classification of F8V, 4% more massive than the Sun.
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Nu1 Canis Majoris (ν1 Canis Majoris) is a binary star in the constellation Canis Major. It is visible to the naked eye with a combined apparent visual magnitude of 5.7. Based on parallax shift of 12.366 mas as seen from our orbit, this system is approximately 264 light years from the Sun. As of 2011, the pair had an angular separation of 17.29 arc seconds along a position angle of 264.2°.
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Epsilon Scuti, Latinized from ε Scuti, is a probable astrometric binary star system in the constellation Scutum. It is faintly visible to the naked eye with an apparent visual magnitude of +4.88. Based upon an annual parallax shift of 6.06 mas as seen from Earth, it is located approximately 540 light years from the Sun. It is moving closer to the Sun with a radial velocity of −9.8 km/s.
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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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WR20a is a binary star associated with the young, massive cluster Westerlund 2. It was discovered in 2004 to be one of the most massive binary systems known, for which the masses of the components have been accurately measured. Each star in the system has about eighty times the mass of the Sun. It is not clear why this system is located away from the center of the cluster.
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Mu Persei (Mu Per, μ Persei, μ Per) is a binary star in the constellation of Perseus, with an apparent magnitude of +4.16. The primary component is a yellow G-type supergiant. It is approximately 900 light years from Earth. With an effective temperature of about 5400 kelvins and a radius of 53 solar radii, this star has the luminosity of about 2030 times that of the Sun.
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Gamma Sextantis, Latinized as γ Sextantis, is a binary star system in the equatorial constellation of Sextans. The combined apparent visual magnitude of the system is 5.05, which means it is faintly visible to the naked eye. The annual parallax shift is 11.75 mas, indicating a distance of around 280 light years. The two components orbit each other with a period of 77.55 years and a high eccentricity of 0.691.
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14 Lacertae is a binary star system in the northern constellation Lacerta, located around 1,600 light years away. It has the variable star designation V360 Lacertae; 14 Lacertae is the Flamsteed designation. The system is barely visible to the naked eye in good seeing conditions, having a peak apparent visual magnitude of 5.91. It is moving closer to the Earth with a heliocentric radial velocity of −16 km/s.
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Zeta Tauri (ζ Tauri, abbreviated Zeta Tau, ζ Tau) is a binary star in the zodiac constellation of Taurus, the Bull. It has an apparent visual magnitude of 3.0, which is bright enough to be seen with the naked eye. Parallax measurements place it at a distance of roughly 440 light-years from the Sun. The two components are designated Zeta Tauri A (officially named Tianguan ) and B.
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VV Cephei, also known as HD 208816, is an eclipsing binary star system located in the constellation Cepheus, approximately 5,000 light years from Earth. It is both a B[e] star and shell star. VV Cephei is an eclipsing binary with the second longest known period. A red supergiant fills its Roche lobe when closest to a companion blue star, the latter appearing to be on the main sequence.
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Gamma Corvi (γ Corvi, abbreviated Gamma Crv, γ Crv) is a binary star and the brightest star in the southern constellation of Corvus, having an apparent visual magnitude of 2.59. The system's two components are designated Gamma Corvi A (officially named Gienah , traditionally the name of the system)) and Gamma Corvi B. The distance to this system has been measured directly using the parallax technique, yielding an estimated from the Sun.
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Zeta Cancri can be resolved as a binary star in small telescopes. Its binary nature was discovered in 1756 by Tobias Mayer. William Herschel resolved the two components that make up Zeta¹ Cancri in 1781. As early as 1831, John Herschel noticed perturbations in Zeta² Cancri's orbit around Zeta¹; this led Otto Wilhelm von Struve, in 1871, to postulate a fourth, unseen, component which orbited closely the visible member of Zeta².
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Upsilon Ursae Majoris (υ UMa) is the Bayer designation for a binary star in the northern circumpolar constellation of Ursa Major. It is visible to the naked eye with an apparent visual magnitude of +3.79. Based upon an annual parallax shift of 13.24 mas, it is located roughly 246 light years from the Sun. The primary member of the system, component A, is an F-type subgiant star.
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He was elected to the National Academy of Sciences in 1950. He published multiple papers on stellar absolute magnitudes, proper motions, and radial velocities of various stars, along with binary star systems and orbital derivations of spectroscopic binaries. Among his publications was the General Catalogue of Stellar Radial Velocities in 1953. The crater Wilson on the Moon is co-named for him, Alexander Wilson and Charles T. R. Wilson.
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Zeta1 Antliae is the Bayer designation for a binary star system in the southern constellation of Antlia. Based upon parallax measurements, the pair are located at a distance of roughly from Earth. They have apparent magnitudes of +6.20 and +7.01 and are separated by 8.042 arcseconds. The apparent magnitude of the combined system is +5.76, which is bright enough to be seen with the naked eye in suitably dark skies.
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CS Camelopardalis (CS Cam) is a binary star in reflection nebula VdB 14, in the constellation Camelopardalis. It forms a group of stars known as the Camelopardalis R1 association, part of the Cam OB1 association. The near- identical supergiant CE Camelopardalis is located half a degree to the south. The primary component, CS Camelopardalis A, is a blue-white B-type supergiant with a mean apparent magnitude of 4.21m.
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Psi Velorum (ψ Vel, ψ Velorum) is a binary star system in the southern constellation of Vela. Based upon an annual parallax shift of 53.15 mas as seen from Earth, it is located 61.4 light years from the Sun. It is visible to the naked eye with a combined apparent visual magnitude of +3.58. The motion of this system through space makes it a candidate member of the Castor stellar kinematic group.
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52 Sagittarii is a binary star system in the southern constellation of Sagittarius. It has the Bayer designation h2 Sagittarii, while 52 Sagittarii is the Flamsteed designation. This system is visible to the naked eye as a faint, blue-white hued point of light with an apparent visual magnitude of 4.59. It is located approximately 190 light years away based on parallax, but is drifting closer with a radial velocity of −19 km/s.
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Psi Virginis (ψ Vir, ψ Virginis) is a suspected binary star system in the zodiac constellation of Virgo. It can be seen with the naked eye and has an apparent visual magnitude of +4.80. Based upon the annual parallax shift of 5.99 milliarcseconds, the distance to this star is roughly 540 light years. The angular size of Psi Virginis was measured on December 26, 1975 during an occultation by the Moon, yielding the estimate .
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Alpha Comae Berenices (α Comae Berenices, abbreviated Alpha Com, α Com) is a binary star in the constellation of Coma Berenices (Berenice's Hair), away. It consists of two main sequence stars, each a little hotter and more luminous than the Sun. Alpha Comae Berenices is said to represent the crown worn by Queen Berenice. The two components are designated Alpha Comae Berenices A (officially named Diadem , the traditional name for the system) and B.
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Theta1 Sagittarii (θ1 Sagittarii) is a close binary star system in the zodiac constellation of Sagittarius. It is visible to the naked eye with an apparent visual magnitude of 4.37. Based upon an annual parallax shift of 6.29 mas as seen from Earth, this star is located around 520 light years from the Sun. At that distance, the visual magnitude is diminished by an extinction factor of 0.24 due to interstellar dust.
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68 Ophiuchi is a binary star system in the equatorial constellation of Ophiuchus. It is visible to the naked eye as a faint star with an apparent visual magnitude of 4.42. The system is located around distant from the Sun, based on parallax, and is drifting further away with a radial velocity of +6 km/s. This is a spectroscopic binary with an orbital period of 177 years and an eccentricity of 0.83.
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SU Ursae Majoris, or SU UMa, is a close binary star in the northern circumpolar constellation of Ursa Major. It is a periodic cataclysmic variable that varies in magnitude from a peak of 10.8 down to a base of 14.96. The distance to this system, as determined from its annual parallax shift of , is 719 light years. It is moving further from the Earth with a heliocentric radial velocity of +27 km/s.
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The effective temperature of the outer envelope is 14,890 K, with the energy being emitted at this temperature giving it the blue-white hue that is a characteristic of a B-type star. It is rotating rapidly with a projected rotational velocity of 190 km s−1, which gives a lower bound for the actual azimuthal velocity along the star's equator. This is most probably a binary star and may be a triple star system.
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74 Cygni is a visual binary star system in the northern constellation Cygnus, located around 249 light years distant from the Sun. It is visible to the naked eye as a faint, white-hued star with a combined apparent visual magnitude of 5.04. The pair orbit each other with a period of and an eccentricity of 0.5. The system is a source of X-ray emission, which is most likely coming from the secondary component.
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Lightcurve of Gamma Persei's 2019 eclipse recorded by NASA's Transiting Exoplanet Survey Satellite (TESS). Gamma Persei (Gamma Per, γ Persei, γ Per) is a binary star system in the constellation Perseus. The combined apparent visual magnitude of the pair is +2.9, making it the fourth-brightest member of the constellation. The distance to this system has been measured using the parallax technique, giving an estimate of roughly with a 4% margin of error.
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Van der Klis's research focuses on X-ray binaries, pairs of stars orbiting each other that emit X-ray radiation. Some binary star systems contain a compact object like a neutron star or a black hole. By studying the dynamics of materials in the vicinity of such objects one can learn about their mass, radius and rotational speed. Moreover, this kind of research provides a testing ground for cosmology and general relativity.
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Mu Serpentis, Latinized from μ Serpentis, is a binary star in the Serpens Caput (head) section of the equatorial constellation Serpens. It is visible to the naked eye with an apparent visual magnitude of 3.543. Based upon an annual parallax shift of 19.23 mas as seen from Earth, it is located around 170 light years from the Sun. This is an astrometric binary for which coarse orbital elements have been determined based on interferometric observations.
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RR Ursae Minoris, or RR UMi, is a binary star system in the northern circumpolar constellation of Ursa Minor. It can be viewed with the naked eye, typically having an apparent visual magnitude of around 4.710. Based upon an annual parallax shift of as seen from Earth's orbit, it is located 330 light years away. The system is moving further from the Sun with a heliocentric radial velocity of +6 km/s.
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Its two brightest stars, Delta Crateris of magnitude 3.56 and Alpha Crateris of magnitude 4.07, are ageing orange giant stars that are cooler and larger than the Sun. Beta Crateris is a binary star system composed of a white giant star and a white dwarf. Seven star systems have been found to host planets. A few notable galaxies, including Crater 2 and NGC 3981, and a famous quasar lie within the borders of the constellation.
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Delta Columbae is a binary star system in the constellation Columba. It can be seen with the naked eye having an apparent visual magnitude of 3.85. The distance to this system, based upon an annual parallax shift of 13.94 mas, is around 234 lightyears. Delta Columbae was a latter designation of 3 Canis Majoris, as the early astronomers Johann Bayer and John Flamsteed did not include the constellation Columba in their star charts.
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However, S Carinae has a shorter period – 150 days, though it is much more distant at 1300 light- years from Earth. Carina is home to several double stars and binary stars. Upsilon Carinae is a binary star with two blue-white hued giant components, 1600 light-years from Earth. The primary is of magnitude 3.0 and the secondary is of magnitude 6.0; the two components are distinguishable in a small amateur telescope.
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Psi Crateris, Latinized from ψ Crateris, is the Bayer designation for a visual binary star system in the southern constellation of Crater. It is faintly visible to the naked eye with an apparent visual magnitude of 6.13. According to the Bortle scale, it requires dark suburban or rural skies to view. Based upon an annual parallax shift of 6.5 mas, the system is located approximately 500 light years away from the Sun.
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Albireo, designated Beta Cygni, is a celebrated binary star among amateur astronomers for its contrasting hues. The primary is an orange-hued giant star of magnitude 3.1 and the secondary is a blue-green hued star of magnitude 5.1. The system is 380 light- years away and is visible in large binoculars and all amateur telescopes. Gamma Cygni, traditionally named Sadr, is a yellow-tinged supergiant star of magnitude 2.2, 1500 light-years away.
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F Centauri is a suspected astrometric binary star system in the southern constellation of Centaurus. It has a reddish hue and is visible to the naked eye with an apparent visual magnitude that fluctuates around +5.01. The system is located at a distance of approximately 450 light years from the Sun based on parallax, and it has an absolute magnitude of −0.87. O. J. Eggen flagged this star as a member of the Hyades Supercluster.
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5 Tauri is a binary star in the zodiac constellation of Taurus, located approximately 530 light years from the Sun. It is visible to the naked eye as a faint orange-hued star with an apparent visual magnitude of +4.14. It is moving further from the Earth with a heliocentric radial velocity of +14 km/s. This is a spectroscopic binary with a period of 960 days and an eccentricity of about 0.4.
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Light curve of AX Circini recorded by NASA's Transiting Exoplanet Survey Satellite (TESS) AX Circini is a binary star system in the southern constellation of Circinus. It has a nominal magnitude of 5.91, which is bright enough to be visible to the naked eye. Based upon an annual parallax shift of , it is located roughly 1,900 light years from the Earth. The system is moving closer with a heliocentric radial velocity of −21 km/s.
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34 Persei is a binary star system in the northern constellation of Perseus. It is visible to the naked eye as a faint, blue-white hued point of light with a combined apparent visual magnitude of 4.67. The system is located approximately 540 light years away from the Sun based on parallax, but it is drifting closer with a radial velocity of −3.5 km/s. It is a likely member of the Alpha Persei Cluster.
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This is a single-lined spectroscopic binary star system with an orbital period of 15.8 days and an eccentricity of 0.31. The primary member, component A, is an A-type main sequence star with a stellar classification of A1VsSi:. The stellar spectrum has the appearance of a hot Am star, showing overabundances of many iron-peak and heavier elements, but an underabundance of helium. In particular, it has an abnormal abundance of silicon.
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Vega also forms one vertex of a much smaller triangle, along with Epsilon and Zeta Lyrae. Zeta forms a wide binary star visible in binoculars, consisting of an Am star and an F-type subgiant. The Am star has an additional close companion, bringing the total number of stars in the system to three. Epsilon is a more famous wide binary that can even be separated by the naked eye under good conditions.
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Studies of this very rare system have allowed astronomers to measure the Cepheid mass with unprecedented accuracy. However, study of the stars has indicated that there is still a discrepancy between observed mass and theoretical characteristics of this type of binary star. The two stars orbit each other every 309 days, and each has 4.14 solar masses. The primary component having an effective temperature of 5900k and the secondary a temperature of 5080K.
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HD 15524 is a wide binary star in the northern zodiac constellation of Aries. Located approximately away, the primary, a yellow-white subgiant or main sequence star has an apparent magnitude of 5.97, meaning that it can be viewed with the naked eye under good conditions. The secondary, separated from the primary by 12.4 arcseconds, has an apparent magnitude of 10.4. This system is the likely source of X-ray emission coming from these coordinates.
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BD−10°3166 is a K-type main sequence star approximately 268 light-years away in the constellation of Crater. It was inconspicuous enough not be included in the Draper catalog (HD). The Hipparcos satellite also did not study it, so its true distance is poorly known. The distance measured by the Gaia spacecraft of 268 light years rules out a suggested companion star, LP 731-076, being its true binary star companion.
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Pi2 Orionis (π2 Ori, π2 Orionis) is the Bayer designation for a solitary star in the equatorial constellation of Orion. Although the Bright Star Catalogue lists this as a spectroscopic binary star system, this does not appear to be the case. It is visible to the naked eye with an apparent visual magnitude of 4.35. Based upon an annual parallax shift of 14.53 mas, it is located roughly 224 light years away from the Sun.
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Kappa1 Apodis, Latinized from κ1 Apodis, is the Bayer designation for a binary star system in the southern circumpolar constellation of Apus. Based upon parallax measurements, it is located roughly from Earth. The combined apparent visual magnitude of the system is 5.52, indicating that this is a faint, naked eye star that can be viewed in dark suburban skies. It is moving away from the Sun with a radial velocity of +62 km/s.
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GRS 1915+105 or V1487 Aquilae is an X-ray binary star system which features a regular star and a black hole. It was discovered on August 15, 1992 by the WATCH all-sky monitor aboard Granat. "GRS" stands for "GRANAT source", "1915" is the right ascension (19 hours and 15 minutes) and "105" reflects the approximate declination (10 degrees and 56 arcminutes). The near-infrared counterpart was confirmed by spectroscopic observations.
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HD 133002 (HR 5596) is a possible binary star in the northern constellation of Ursa Minor. With an apparent visual magnitude of 5.65, it is faintly visible to the naked eye. (According to the Bortle scale, it can be viewed from dark rural skies.) The high declination of +82.5° means it is hidden from view from most of the southern hemisphere. Parallax measurements yield an estimated distance of around 143 light years from the Sun.
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22 Vulpeculae is a binary star system in the northern constellation Vulpecula. Based on its parallax, it is located some 1,900 light-years away, and it has an apparent magnitude of about 5.176, making it visible to the naked eye. The system is moving closer to the Earth with a heliocentric radial velocity of −23 km/s. The pair have an orbital period of in what is assumed to be a circular orbit.
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Tau Cygni, Latinised from τ Cygni, is a binary star system in the constellation Cygnus, approximately 69 light years away from Earth. This visual binary system has a period of 49.6 years. The main star, 4th magnitude GJ 822.1 A, is a yellowish white subgiant star of the spectral type F2IV. It therefore has a surface temperature of 6,000 to 7,500 kelvins and is larger, hotter, and several times as bright as the Sun.
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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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83 Ursae Majoris is a candidate binary star system in the northern circumpolar constellation of Ursa Major. This is a semiregular variable star, like Mira; for that reason it has been given the variable star designation IQ Ursae Majoris. It ranges in brightness from apparent visual magnitude 4.69 to 4.75. Percy and Au (1994) identified it as a small amplitude red variable with an irregular behavior, having a characteristic time scale of 20 days.
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Based upon its parallax measurement of , this star is located approximately 520 light years from Earth. It is visible to the naked eye as a faint, orange-hued star with an apparent visual magnitude of 4.89. 1 Aurigae is moving closer to the Earth with a heliocentric radial velocity of −25 km/s. This is a possible binary star system, based upon the status of the visible component as a mild barium star.
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89 Aquarii (abbreviated 89 Aqr) is a binary star system in the equatorial constellation of Aquarius. 89 Aquarii is the Flamsteed designation, though it also bears the Bayer designation c3 Aquarii. database record, HD-DM-GC-HR-HIP- Bayer-Flamsteed Cross Index, N. D. Kostjuk, Institute of Astronomy of Russian Academy of Sciences, 2002; CDS ID IV/27A. The apparent visual magnitude of +4.69 is bright enough to be seen with the naked eye.
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1 Aquarii is a binary star system in the zodiac constellation of Aquarius, about 257 light years away from the Sun. 1 Aquarii is the Flamsteed designation. It is visible to the naked eye as a faint, orange-hued star with an apparent visual magnitude of 5.151, located a degree north of the celestial equator. The system is moving closer to the Earth with a heliocentric radial velocity of −41 km/s.
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47 Andromedae is a binary star system in the northern constellation of Andromeda. The designation is from the star catalogue of John Flamsteed, first published in 1712. The system has a combined apparent visual magnitude of 5.60, which is just bright enough to be faintly visible to the naked eye under good seeing conditions. The distance to this system, as determined from an annual parallax shift of 15.9805 mas, is about 204 light years.
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9 Andromedae, abbreviated 9 And by convention, is a variable binary star system in the northern constellation Andromeda. 9 Andromedae is the Flamsteed designation, while it bears the variable star designation AN Andromedae, or AN And. The maximum apparent visual magnitude of the system is 5.98, which places it near the lower limit of visibility to the human eye. Based upon an annual parallax shift of , it is located 460 light years from the Earth.
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66 Andromedae is a binary star system in the northern constellation of Andromeda, near the northern border with Perseus. The designation is from the star catalogue of English astronomer John Flamsteed, first published in 1712. It has a combined apparent magnitude of 6.16, which is near the lower limit of stars that are visible to the naked eye under good seeing conditions. An annual parallax shift of provides a distance estimate of 178 light years.
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6 Boötis is a binary star system in the northern constellation of Boötes, located around 460 light years away from the Sun. It has the Bayer designation e Boötis; 6 Boötis is the Flamsteed designation. The system is visible to the naked eye as a faint, orange-hued star with an apparent visual magnitude of 4.92. It is moving closer to the Earth with a heliocentric radial velocity of −3 km/s.
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47 Boötis is a binary star system in the northern constellation of Boötes, located 261 light years away from the Sun. It has the Bayer designation k Boötis; 47 Boötis is the Flamsteed designation. The system is visible to the naked eye as a faint, white-hued star with a combined apparent visual magnitude of 5.58. It is moving closer to the Earth with a heliocentric radial velocity of −13 km/s.
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At its present distance, the visual magnitude is diminished by an extinction factor of 0.135 due to interstellar dust. Xi Cancri is a single-lined spectroscopic binary star system with an orbital period of 4.66 years, an eccentricity of 0.06, and a semimajor axis of 0.01 arcseconds. The primary, Xi Cancri A, is a yellow G-type giant with an apparent magnitude of +5.70. Its companion, Xi Cancri B, is of magnitude 6.20.
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1 Centauri, or i Centauri, is a yellow-white hued binary star system in the southern constellation Centaurus. It can be seen with the naked eye, having an apparent visual magnitude of +4.23. Based upon an annual parallax shift of 51.54 mas as seen from Earth's orbit, it is located 51.5 light years from the Sun. The system is moving closer to the Sun with a radial velocity of −21.5 km/s.
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Kappa Centauri (κ Cen, κ Centauri) is a binary star in the southern constellation of Centaurus. With an apparent visual magnitude of +3.14, it can be viewed with the naked eye on a dark night. Parallax measurements place it at an estimated distance of from Earth. This is a spectroscopic binary system where the presence of an orbiting companion is revealed by shifts in the absorption lines caused by the Doppler effect.
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Upsilon2 Centauri (υ2 Centauri) is a binary star system in the southern constellation Centaurus. It is visible to the naked eye with an apparent visual magnitude of +4.33. Based upon an annual parallax shift of just 2.57 mas as seen from Earth, this star is located roughly 1,300 light years from the Sun. Relative to its neighbors, the system has a peculiar velocity of and it may form a runaway star system.
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This is not a binary star system in the sense of having a gravitationally-bound stellar companion. However, in early 2004, a brown dwarf companion Nu Ophiuchi b was discovered. This sub-stellar companion has at least 21.9 times the mass of Jupiter and takes 536 days (1.47 years) to complete an orbit. A second brown dwarf companion was discovered in 2010, orbiting further from the star with a period of 3,169 days (8.68 years).
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Delta1 Telescopii is a blue-white hued binary star system in the southern constellation of Telescopium. It is faintly visible to the naked eye, having an apparent visual magnitude of 4.94. Based upon an annual parallax shift of 4.61 mas as seen from Earth, this system is roughly 710 light years from the Sun. At that distance, the visual magnitude is diminished by an extinction factor of 0.29 due to interstellar dust.
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Sigma Geminorum (σ Gem) is a binary star system in the constellation Gemini, just to the northeast of Pollux. It is visible to the naked eye with an apparent visual magnitude of 4.20. Based upon an annual parallax shift of 26.08 mas, it is located 125 light years from the Sun. Sigma Geminorum is a single-lined spectroscopic binary, which means that the spectrum of only one of the components can be discerned.
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HD 158614 is a spectroscopic binary star system approximately 60 light-years away in the constellation of Ophiuchus. This system is in the Zeta Herculis moving group, which is of low metallicity stars, 5 billion years old. Besides ζ Herculis, the group includes δ Trianguli, ζ Reticuli, 1 Hydrae, Gl 456, φ2 Pavonis, and GJ 9079. This binary was included in a search for brown dwarfs that turned up no large companions.
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HD 170469 is a probable binary star system in the equatorial constellation of Ophiuchus. It is too faint to be viewed with the naked eye, having an apparent visual magnitude of 8.21. The system is located at a distance of 197 light years away from the Sun based on parallax. It is drifting closer with a radial velocity of −59 km/s, and is expected to come to within in about 959,000 years.
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HD 11964 is a binary star system located 110 light-years away from the Sun in the equatorial constellation of Cetus. It is visible in binoculars or a telescope but is too faint to be seen with the naked eye, having an apparent visual magnitude of 7.51. The system is drifting closer to the Sun with a radial velocity of −9 km/s. Two extrasolar planets have been confirmed to orbit the primary.
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30 Geminorum is a suspected astrometric binary star system in the northern zodiac constellation of Gemini. It is visible to the naked eye as a faint, orange-hued point of light with an apparent visual magnitude of 4.49. The distance to this star, as estimated through the use of parallax, is about 299 light years. It is drifting further away from the Sun with a heliocentric radial velocity of +9.5 km/s.
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AN Ursae Majoris is a binary star system in the northern circumpolar constellation of Ursa Major. It is a variable star, with AN Ursae Majoris being the variable star designation, and ranges in brightness from 14.90 down to 20.2. Even at its peak brightness though, the system is much to faint to be visible to the naked eye. Based on parallax measurements, the system is located roughly 1,050 light years away from the Sun.
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HD 81817 is a binary star system in the northern circumpolar constellation of Draco. It has an orange hue and is visible to the naked eye with an apparent visual magnitude of 4.28. The system is located at a distance of approximately 990 light years from the Sun based on parallax, and is drifting closer with a radial velocity of −7 km/s. It is a member of the IC 2391 moving group.
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2MASS J18082002−5104378 (abbreviated J1808−5104) is an ultra metal-poor (UMP) binary star system, in the constellation Ara, about from Earth, and is a single-lined spectroscopic binary (SB1). It is one of the oldest stars in the universe, about 13.53 billion years old, possibly one of the first stars, a star made almost entirely of materials released from the Big Bang. A tiny unseen companion, a low-mass UMP star, is particularly unusual.
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It shines with 4.6 times the luminosity of the Sun. The outer atmosphere is radiating this energy at an effective temperature of 6,725 K, giving it the yellow-white hue of an F-type star. There is some evidence that this may be a binary star system consisting of two stars with identical masses. Examination of Lambda Arae with the Spitzer Space Telescope shows an excess of infrared emission at a wavelength of 70 μm.
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16 Lyrae is a suspected astrometric binary star system in the constellation Lyra, located 126 light years away from the Sun based on parallax. It is visible to the naked eye as a dim, white-hued star with a combined apparent visual magnitude of 5.00. The system is moving further away from the Earth with a heliocentric radial velocity of +5 km/s. It is a suspected member of the Ursa Major Moving Group stream.
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Iota Arietis (ι Ari, ι Arietis) is the Bayer designation for a binary star system in the northern constellation of Aries. It has an apparent visual magnitude of 5.117; bright enough to be dimly seen with the naked eye. Parallax measurements made during the Hipparcos mission yield an estimated distance of from Earth. This is a spectroscopic binary system with an orbital period of 1,568 days (4.3 years) and an eccentricity of 0.36.
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HD 70930 is a binary star system in the southern constellation of Vela. It has the Bayer designation B Velorum, while HD 70930 is the star's identifier in the Henry Draper catalogue. With a combined apparent visual magnitude of 4.79, it is visible to the naked eye as a faint point of light. The distance to this system is approximately 1,700 light years based on parallax, and it has an absolute magnitude of −3.74.
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Delta1 Lyrae, Latinized from δ1 Lyrae, is a binary star system in the constellation Lyra, approximately 1,100 light years away from Earth. The two stars complete an orbit around each other about once every 88 days. They are a spectroscopic binary, meaning the separation between the two is very small, and their orbital velocity is very high. The primary member, component A, is a bluish white main-sequence star of the spectral type B2.5V.
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Kappa Aquarii (κ Aquarii, abbreviated Kappa Aqr, κ Aqr) is a probable binary star in the equatorial constellation of Aquarius. This system is visible to the naked eye, but it is faint at an apparent magnitude of 5.03. Based upon parallax measurements made during the Hipparcos mission, it is around from the Sun. The two components are designated Kappa Aquarii A (formally named Situla , the traditional name for the system) and B.
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Kappa Aquarii is most probably a wide binary star system. The brighter component is a giant star with a stellar classification of K2 III. It has exhausted the supply of hydrogen at its core and has expanded to 13 times the radius of the Sun. It is radiating 60 times the Sun's luminosity from its outer envelope at an effective temperature of 4,581 K, giving it the orange- hued glow of a K-type star.
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Alpha Octantis is a binary star system in the constellation of Octans. The name is Latinized from α Octantis. Despite being labeled the "alpha" star by Johann Bayer in his star atlas Uranometria, it is not the brightest star in the constellation – that title belongs to Nu Octantis. It is visible to the naked eye as a faint, yellow-white hued point of light with an overall apparent visual magnitude of approximately 5.13.
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Eta Draconis (η Draconis, abbreviated Eta Dra, η Dra) is a binary star in the northern circumpolar constellation of Draco. Despite having an apparent visual magnitude of only +2.73, it is the second-brightest star in this generally faint constellation. Based upon parallax measurements collected during the Hipparcos mission, this star is located at a distance of about from the Sun. The two components are designated Eta Draconis A (also named Athebyne ) and B.
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In astronomy, a common envelope (CE) is gas that contains a binary star system. The gas does not rotate at the same rate as the embedded binary system. A system with such a configuration is said to be in a common envelope phase or undergoing common envelope evolution. During a common envelope phase the embedded binary system is subject to drag forces from the envelope which cause the separation of the two stars to decrease.
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Phi Aquarii, Latinized from φ Aquarii, is the Bayer designation for a binary star system in the equatorial constellation of Aquarius. It is visible to the naked eye with a combined apparent visual magnitude of +4.223. Parallax measurements indicate its estimated distance from Earth is roughly , and it is drifting further away with a radial velocity of +2.5 km/s. The proximity of this star to the ecliptic means it is subject to lunar occultations.
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111 Herculis is a suspected astrometric binary star system located 92 light years from the Sun in the northern constellation Hercules. It is visible to the naked eye as a faint, white-hued point of light with an apparent visual magnitude of 4.34. The system is moving nearer to the Earth with a heliocentric radial velocity of −45 km/s, and may come as close as in 537,000 years. According to Cowley et al.
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Rho Aquarii, Latinized from ρ Aquarii, is the Bayer designation for a binary star in the equatorial constellation of Aquarius. It is visible to the naked eye with an apparent visual magnitude of +5.34. Based upon parallax measurements made during the Hipparcos mission, this star is at a distance of roughly from Earth. This is a single-lined spectroscopic binary, with the presence of a companion being revealed by Doppler shifts in the spectrum.
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AE Aquarii is a cataclysmic variable binary star of the DQ Herculis type. Based upon parallax measurements, the system is located at a distance of about from the Earth. Because of its unique properties, this system has been subject to a number of scientific studies. The AE Aquarii system consisting of an ordinary star in a close orbit around a magnetic white dwarf; the pair orbit each other with a period of 9.88 hours.
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12 Hydrae is a probable astrometric binary star system located 202 light years away from the Sun in the equatorial constellation of Hydra. It has the Bayer designation D Hydrae; 12 Hydrae is the Flamsteed designation. This system is visible to the naked eye as a faint, yellow-hued star with a combined apparent visual magnitude of 4.32. It is moving closer to the Earth with a heliocentric radial velocity of −8.5 km/s.
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Pi Cassiopeiae, Latinized from π Cassiopeiae, is a close binary star system in the constellation Cassiopeia. It is visible to the naked eye with an apparent visual magnitude of +4.949. Based upon an annual parallax shift of 18.63 mas as seen from Earth, this system is located about 175 light years from the Sun. This is a double-lined spectroscopic binary system with an orbital period of nearly two days in a circular orbit.
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"Binary Star" was used at the opening theme for the anime Legend of the Galactic Heroes: Die Neue These – Encounter, while "Cage" was used at the theme song for the life-sized Unicorn Gundam statue from Mobile Suit Gundam Unicorn. "narrative" was used as the theme song for the anime film Mobile Suit Gundam Narrative. "ME & CREED " will be used as the theme song for the upcoming mobile game Blue Exorcist: Damned Chord.
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72 Ophiuchi is a binary star system in the equatorial constellation of Ophiuchus. It is visible to the naked eye as a faint, white-hued point of light with a combined apparent visual magnitude of 3.73. It is located approximately 86.9 light years away from the Sun based on parallax, but is moving closer with a heliocentric radial velocity of -23.9 km/s. As of 2008, the pair had an angular separation of .
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This system is located around 15,500 light-years away from Earth. A recurrent nova, it has brightened to the 7th magnitude in the years 1890, 1902, 1920, 1944, 1966 and 2011 from a baseline of around 14th magnitude. These outbursts are thought to be due to the white dwarf accreting material from its companion and ejecting periodically. TY Pyxidis is an eclipsing binary star whose apparent magnitude ranges from 6.85 to 7.5 over 3.2 days.
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Equuleus contains some double stars of interest. γ Equ consists of a primary star with a magnitude around 4.7 (slightly variable) and a secondary star of magnitude 11.6, separated by 2 arcseconds. Epsilon Equulei is a triple star also designated 1 Equulei. The system, 197 light-years away, has a primary of magnitude 5.4 that is itself a binary star; its components are of magnitude 6.0 and 6.3 and have a period of 101 years.
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The secondary is of magnitude 7.4 and is visible in small telescopes. The components of the primary are becoming closer together and will not be divisible in amateur telescopes beginning in 2015. δ Equ is a binary star with an orbital period of 5.7 years, which at one time was the shortest known orbital period for an optical binary. The two components of the system are never more than 0.35 arcseconds apart.
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QV Normae, also known as Norma X-2, is a high mass X-ray binary star system in the constellation Norma. It varies between apparent magnitudes of 16.19 and 16.31. The X-ray source was first identified in the early 1970s. The nature of the system was discovered in 1978 by astronomers who aligned a visual source of a reddened hot blue-white star with the X-ray source 4U 1538 - 52.
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She reported the discovery of several objects of sub-stellar mass and proposed a 0.01 solar-mass planetary companion to the star Lalande 21185 in 1951. The same proposal of planetary objects was made for a number of other stars as well. Claims for the smaller planetary objects were never confirmed and gradually have become discredited. However, she was quite successful in using the same techniques for characterizing many binary star systems.
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Imara works with the Banneker Institute at Harvard, and is a member of the Breakthrough Starshot research team. Her work investigates the structure and evolution of stellar nurseries in both the Milky Way Galaxy and other galaxies throughout the universe, and she has developed a model that connects galaxy mass, star formation rates and dust temperatures. Together with Rosanne Di Stefano, Imara has proposed a method for detecting exoplanets in X-ray binary star systems.
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Reflection nebula around HD 87643 HD 87643 is a B[e] class binary star embedded in a reflection nebula. The system is described as having "one of the most extreme infrared excesses for this object class. It harbours a large amount of both hot and cold dust, and is surrounded by an extended reflection nebula." and is important for astronomers in their study of stellar formation. All the properties of HD 87643 are highly uncertain.
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66 Tauri, also known as r Tauri, is a binary star in the constellation of Taurus. The combined apparent magnitude of the system is 5.098, with the magnitudes of the two components being 5.8 and 5.9, respectively. Parallax measurements by Hipparcos put 66 Tauri at some 400 light-years (121 parsecs) away. This is a visual binary where the positions of the two stars are tracked over time, and used to calculate an orbit.
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Gamma Librae (γ Librae, abbreviated Gamma Lib, γ Lib) is a suspected binary star system in the constellation of Libra. It is visible to the naked eye, having an apparent visual magnitude of +3.91. Based upon an annual parallax shift of 19.99 mas as seen from Earth, it lies 163 light years from the Sun. The primary component (designated Gamma Librae A) has been formally named Zubenelhakrabi , the traditional name of the system.
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Zeta Draconis (ζ Draconis, abbreviated Zet Dra, ζ Dra) is a binary star in the northern circumpolar constellation of Draco. With an apparent visual magnitude of +3.17, it is the fifth-brightest member of this generally faint constellation. Its distance from the Sun has been measured using the parallax technique, yielding an estimate of roughly . The two components are designated Zeta Draconis A (formally named Aldhibah , after the traditional name of the system) and B.
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Xi Phoenicis, Latinized from ξ Phoenicis, is a visual binary star system in the southern constellation of Phoenix. It is faintly visible to the naked eye, having an apparent visual magnitude of 5.70. Based upon an annual parallax shift of 14.61 mas as measured from Earth, it is located around 223 light years from the Sun. The system is moving away from the Sun with a radial velocity of about +10 km/s.
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In addition to having the current southern pole star of Earth, Octans also contains the southern pole star of the planet Saturn, which is the magnitude 4.3 Delta Octantis. The Astronomical Society of Southern Africa in 2003 reported that observations of the Mira variable stars R and T Octantis were urgently needed. Three star systems are known to have planets. Mu2 Octantis is a binary star system, the brighter component of which has a planet.
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LB-1 is a binary star system in the constellation Gemini. It is composed of a B-type star and an unseen object that might be a black hole. If the star is an ordinary main sequence B-type star (with its luminosity in conflict with a mainstay astronomic satellite's parallax measurements), the companion which is strongly suspected to be solitary, would be a black hole having mass outside of ordinary single stellar evolution parameters.
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17 Sagittarii is a binary star system in the zodiac constellation of Sagittarius, located 675 light years from the Sun. With a combined apparent visual magnitude of 6.89 it is below the normal limit of visibility to the naked eye. The system is moving closer to the Earth with a heliocentric radial velocity of −14 km/s. J. Allen Hynek (1938) found an initial spectral type of G5 + A5 for the pair.
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Sigma Puppis (Sigma Pup, σ Puppis, σ Pup) is a binary star system in the southern constellation of Puppis. It has an apparent visual magnitude of 3.25, which is bright enough to be visible to the naked eye at night from the southern hemisphere. Through a telescope, it appears as a bright, orange-hued star with a nearby white companion. Parallax measurements indicate this star is located at a distance of about from Earth.
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Nu Leporis, Latinized from ν Leporis, is a probable astrometric binary star system in the constellation Lepus. It is visible to the naked eye as a faint star with an apparent visual magnitude of 5.29. Based upon an annual parallax shift of 7.70 mas as seen from the Earth, it is 420 light years from the Sun. The visible component is a B-type star with an estimated 3.3 times the mass of the Sun.
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The telescopes were used to observe the star's light, thereby detecting times when WASP-24b might have transited its star. The Faulkes telescopes collected data on two complete transits and one partial one. During this period, a nearby eclipsing binary star called N1 was considered and avoided to avoid contaminating the collected light samples. Information collected by the Faulkes telescopes was extrapolated to reveal the characteristics of the star, and from there of the planet.
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The inner pair form a binary star system with an orbital period of 192 years and an eccentricity of 0.611. Both components are A-type main- sequence stars, indicating that they are generating energy through core hydrogen fusion. The brighter member of this pair, designated component A, is the primary for the system with a visual magnitude of 4.18 and a stellar classification of A0V. The secondary, component B, is magnitude 5.22 and class A4V.
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Gamma Cassiopeiae, Latinized from γ Cassiopeiae, is a star at the center of the distinctive "W" asterism in the northern circumpolar constellation of Cassiopeia. Although it is a fairly bright star with an apparent visual magnitude that varies from 1.6 to 3.0, it has no traditional Arabic or Latin name. It sometimes goes by the informal name Navi. Gamma Cassiopeiae is a Be star, a variable star, and a binary star system.
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Beta Octantis, Latinized from β Octantis, is a probable astrometric binary star system in the southern circumpolar constellation of Octans. It is faintly visible to the naked eye with an apparent visual magnitude of 4.13. Based upon an annual parallax shift of 21.85 mas as seen from Earth, it is located about 149 light years from the Sun. It is moving away from the Sun with a radial velocity of +19 km/s.
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Delta Cassiopeiae is a possible eclipsing binary star system consisting of a pair of stars that orbit about each other over a period of 759 days. The combined apparent visual magnitude of the two stars is 2.68, making it readily observable with the naked eye. Eclipses have been reported with a period of 759 days, when the brightness drops by 0.07 magnitudes. Modern studies have shown no brightness variations greater than 0.01 magnitudes.
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They can be separated in small telescopes. A third star, Beta3 Tucanae, is separated by 10 arcminutes from the two, and able to be seen as a separate star with the unaided eye. Each star is itself a binary star, making six in total. Lying in the southwestern corner of the constellation around 251 light- years away from Earth, Delta Tucanae consists of a blue-white primary contrasting with a yellowish companion.
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Beta Aurigae (Latinized from β Aurigae, abbreviated Beta Aur, β Aur), officially named Menkalinan , is a binary star system in the northern constellation of Auriga. The combined apparent visual magnitude of the system is 1.9, making it the second-brightest member of the constellation after Capella. Using the parallax measurements made during the Hipparcos mission, the distance to this star system can be estimated as , give or take a half- light-year margin of error.
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29 Vulpeculae is a suspected astrometric binary star system in the northern constellation Vulpecula. It is visible to the naked eye as a faint, white-hued point of light with an apparent visual magnitude of 4.82. The system lies approximately 209 light years away from the Sun based on parallax, and is a member of the IC 2391 supercluster. It is moving closer to the Earth with a heliocentric radial velocity of −17 km/s.
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PSR B1620−26 is a binary star system located at a distance of 3,800 parsecs (12,400 light-years) in the globular cluster of Messier 4 (M4, NGC 6121) in the constellation of Scorpius. The system is composed of a pulsar (PSR B1620−26 A) and a white dwarf star (WD B1620−26) or PSR B1620−26 B). As of 2000, the system is also confirmed to have an exoplanet orbiting the two stars.
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45 Cancri is a binary star system in the zodiac constellation of Cancer, located 680 light years away from the Sun. It has the Bayer designation A1 Cancri; 45 Cancri is the Flamsteed designation. It is visible to the naked eye as a faint, white-hued star at an apparent visual magnitude of 5.62. The pair form a double-lined spectroscopic binary with an orbital period of and an eccentricity of 0.46.
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HD 22663 (y Eridani) is a candidate astrometric binary star system in the equatorial constellation of Eridanus. It is visible to the naked eye with an apparent visual magnitude of 4.57. Based upon an annual parallax shift of , it is located around 230 light years from the Sun. It is moving further away from the Earth with a heliocentric radial velocity of +11.5 km/s, having come within some 3.76 million years ago.
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Masters of the Universe is the second and final studio album from American hip hop duo Binary Star (Senim Silla & One Be Lo). The release is a remixed and rearranged version of their 1999 debut Waterworld. The album was one of the most acclaimed underground hip hop releases of 2000, though it only sold around 20,000 copies. Masters of the Universe was re-released on July 25, 2006 by Infinite Rhythm Network.
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39 Draconis is a wide binary star system in the northern circumpolar constellation of Draco. It has the Bayer designation b Draconis, while 39 Draconis is the Flamsteed designation. This system is visible to the naked eye as a dim, white-hued point of light with an apparent visual magnitude of 5.0. Parallax measurements made by the Hipparcos spacecraft put it at a distance of 184 light-years, or 56 parsecs away from the Sun.
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Pi Canis Majoris (π Canis Majoris) is a binary star system in the southern constellation of Canis Major. It is visible to the naked eye, having an apparent visual magnitude of +4.69. Based upon an annual parallax shift of 33.80 mas as seen from Earth, this system is located 96.5 light years from the Sun. The star is moving in the general direction of the Sun with a radial velocity of −37.9 km/s.
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Xi Coronae Borealis (ξ CrB) is a binary star system in the northern constellation of Corona Borealis. It is visible to the naked eye with a combined apparent visual magnitude of 4.85. Based upon an annual parallax shift of 17.78 mas as seen from the Earth, it is located about 183 light years from the Sun. As of 2009, the pair had an angular separation of 91 mas along a position angle of 139.4°.
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Gamma Coronae Borealis, Latinized from γ Coronae Borealis, is a binary star system in the northern constellation of Corona Borealis. It is visible to the naked eye with an apparent visual magnitude of 3.83. Based upon an annual parallax shift of 22.33 mas as seen from Earth, it is located about 146 light years from the Sun. The system is moving closer to the Sun with a radial velocity of about −15 km/s.
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HD 216446 is a binary star system in the northern circumpolar constellation of Cepheus. It is faintly visible to the naked eye with a combined apparent visual magnitude of 4.77. The system is located at a distance of approximately 319 light years from the Sun based on parallax, but is drifting closer with a radial velocity of −32 km/s. It is predicted to come to within in around 1.876 million years.
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Epsilon Sculptoris (ε Scl, ε Sculptoris) is a binary star in the constellation Sculptor. It is approximately 91.7 light years from Earth. The primary component, Epsilon Sculptoris A, is a yellow-white F-type main-sequence star with an apparent magnitude of +5.29. Orbiting it with a separation of 4.6 arcseconds, or at least 125 Astronomical Units, is Epsilon Sculptoris B, a yellow G-type main sequence dwarf with an apparent magnitude of +8.6.
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12 Comae Berenices is a binary star system in the northern constellation of Coma Berenices. It is the brightest member of the Coma Cluster and is visible to the naked eye with an apparent visual magnitude of 4.80. Although listed as a suspected variable star, there is no photometric evidence of it being variable in luminosity. However, the radial velocity was found to be variable, as announced by W. W. Campbell in 1910.
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HD 106760 is a single-lined spectroscopic binary star system in the northern constellation of Coma Berenices. It is faintly visible to the naked eye, having an apparent visual magnitude of 4.99. The system is located around 38 light years away, as determined from its annual parallax shift of . It is moving closer with a heliocentric radial velocity of −40 km/s, and is expected to come as close as in about 772,000 years.
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Alpha Tucanae (α Tuc, α Tucanae) is a binary star system in the southern circumpolar constellation of Tucana. With an apparent visual magnitude of 2.86, it can be seen with the naked eye from the southern hemisphere. Using parallax measurements, the distance to this system can be estimated as . A cool star with a surface temperature of 4300 K, it is 424 times as luminous as the sun and 37 times its diameter.
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HR 178 is a probable binary star in the constellation Andromeda. Located approximately distant, it is an evolved Am star with a combined apparent magnitude of 6.06, meaning that it can only be seen with the naked eye on dark, clear nights. The star is suspected of variability, possibly varying between magnitudes 6.04 and 6.06. The spectrum of HR 178 has been extensively studied for establishing element abundances in the evolved Am stars.
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KIC 9832227 is a contact binary star system in the constellation Cygnus, located about 1,940 ± 30 light-years away. It is also identified as an eclipsing binary with an orbital period of almost 11 hours. In 2017, the system was predicted to result in a merger in 2022.2 (± 0.6 years), producing a luminous red nova (LRN) reaching an apparent magnitude of 2. The LRN would remain visible to the naked eye for roughly a month.
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Iota Trianguli Australis (ι Trianguli Australis) is a binary star system in the constellation Triangulum Australe. It is visible to the naked eye with a combined apparent visual magnitude of +5.27. Based upon an annual parallax shift of 25.77 mas as seen from the Earth, it is located around 127 light years from the Sun. The system appears to be moving closer to the Sun with a radial velocity of around −6 km/s.
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HD 222109 is a binary star system in the northern constellation of Andromeda. They have a combined apparent visual magnitude of 5.80, making them visible by the naked eye as a single star. They also have a combined spectral classification B8V. The pair is located at approximately 800 light years from Solar System, and orbit each other with a period of 351.22 years, a separation of 0.41″, and an orbital eccentricity of 0.39.
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ET Andromedae is a binary star system star in the northern constellation of Andromeda. It has an apparent visual magnitude of 6.48, placing it at the nominal limit for visibility with the naked eye. The distance to this system can be estimated from its annual parallax shift of , which yields a value of 602 light years. Variations in the radial velocity of this star suggest it is a single-lined spectroscopic binary system.
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HD 6114 is a visual binary star system in the northern constellation of Andromeda. With a combined apparent magnitude of 6.46, the star can only be seen with the naked eye by keen-eyed observers even on the best of nights. Based upon an annual parallax shift of as seen from Earth's orbit, the system is located approximately distant. The binary nature of this system was discovered by O. Struve in 1864.
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22 Camelopardalis is a binary star system in the northern circumpolar constellation of Camelopardalis, located 212 light years away from the Sun. It has an apparent visual magnitude of 7.03, which is below the normal limit for visibility with the naked eye. This object is moving further from the Earth with a mean heliocentric radial velocity of +10 km/s. Eggen (1991) listed it as a member of the IC 2391 supercluster.
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However, the team was unable to confirm the planet until extensive follow-up observations, as high-resolution imaging resolved the star Kepler-14 as a closely orbiting binary system. The Kepler team would have not noticed that Kepler-14 was a binary star based solely on initial radial velocity measurements (a standard method for confirming a planet's existence), and found that if they had not realized this, their data on Kepler-14b would have been very inaccurate.
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Beta1 Sagittarii, Latinized from β1 Sagittarii, is a binary star system in the zodiac constellation of Sagittarius, next to the southern constellation border with Telescopium. The brighter primary is named Arkab Prior , the traditional name of the system. It is visible to the naked eye with a combined apparent visual magnitude of +4.01. Based upon an annual parallax shift of 10.40 mas as seen from Earth, it is located roughly 310 light-years from the Sun.
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Alpha Volantis (α Vol, α Volantis) is a binary star system in the southern constellation Volans. It has an apparent visual magnitude of +4.00, which is bright enough to be seen with the naked eye. Based upon parallax measurements made with the Hipparcos spacecraft, it is located at a distance of 125 light years from the Sun. As of 2010, the two components of this system had an angular separation of 0.0318″ along a position angle of 286.9°.
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Omega Piscium (Omega Psc, ω Piscium, ω Psc) is a star approximately 106 light years away from Earth, in the constellation Pisces. It has a spectral type of F4IV, meaning it is a subgiant/dwarf star, and it has a temperature of 6,600 kelvins. It may or may not be a close binary star system. Variations in its spectrum were once interpreted as giving it an orbital period of 2.16 days, but this claim was later debunked as false.
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HD 59686 is a binary star system in the northern constellation of Gemini. It is visible to the naked eye as a dim point of light with an apparent visual magnitude of +5.45. The distance to this system is approximately 292 light years based on parallax, but it is drifting closer with a radial velocity of −34 km/s. This is a single-lined spectroscopic binary system with an orbital period of and a high eccentricity of 0.73.
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Pi1 Ursae Minoris is a common proper motion binary star system in the northern circumpolar constellation of Ursa Minor. The pair have apparent visual magnitudes of +6.58 and +7.31, with a combined magnitude of 6.1. They are located about 71 light years from the Sun. The two have an angular separation of 31.4 arc seconds, which corresponds to a physical separation of about 680 AU, and orbit each other with a period of about 13,100 years.
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Pi2 Ursae Minoris (π2 UMi) is a binary star system in the northern circumpolar constellation of Ursa Minor. The pair have apparent magnitudes of 7.32 and 8.15, placing them below the brightness limit of stars that can be readily viewed with the naked eye. They are located about 390 light-years (120 parsecs) away from the Sun. The two have an angular separation of 0.464″ on average, and they orbit each other with a period of about 170 years.
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40 Persei is a wide binary star system in the northern constellation of Perseus. It has the Bayer designation ο Persei, while 40 Persei is the Flamsteed designation. The system is visible to the naked eye as a faint, blue-white hued point of light with an apparent visual magnitude of 4.97. It is located approximately 1060 light years away from the Sun based on parallax, and is drifting further away with a radial velocity of +22 km/s.
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How eclipsing binaries vary in brightness Extrinsic variables have variations in their brightness, as seen by terrestrial observers, due to some external source. One of the most common reasons for this is the presence of a binary companion star, so that the two together form a binary star. When seen from certain angles, one star may eclipse the other, causing a reduction in brightness. One of the most famous eclipsing binaries is Algol, or Beta Persei (β Per).
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Gallifrey () is a fictional planet in the long-running British science fiction television series Doctor Who. It is the original home world of the Time Lords, the civilisation to which the main protagonist, the Doctor belongs. It is located in a binary star system 250 million light years from Earth. It was first shown in The War Games (1969) during the Second Doctor's trial though was not identified by name until The Time Warrior (1973–74).
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The constellation of Reticulum, the net, as it can be seen by the naked eye Only two of the stars in this constellation are brighter than visual magnitude 5: Alpha (α) and Beta (β) reticuli. The reddish star R Reticuli is a Mira variable. This variable was discovered by C. Ragoonatha Chary at the Madras Observatory in India. The binary star system Epsilon Reticuli consists of a spectral class K2IV star being orbited by a white dwarf.
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Based on parallax measurements, this system is located about 50 light years from the Sun. In 2000, a planetary companion was announced, orbiting the star ε Reticuli A. Zeta Reticuli is a wide binary star system, with both members being similar to the Sun. It is located at a distance of about 39 light years. This system gained some notoriety in ufology when the alleged alien abductees Betty and Barney Hill named it as the home of their abductors.
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This name was later connected by Allen with 46 Leonis Minoris—an error perpetuated by subsequent astronomers. The original "Praecipua", 37 Leonis Minoris, has an apparent magnitude of 4.69, but is a distant yellow supergiant of spectral type G2.5IIa and absolute magnitude of −1.84, around distant. Leo Minor as seen by the naked eye Beta Leonis Minoris is a binary star system. The primary is a giant star of spectral class G8 and apparent magnitude of 4.4.
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LSI+61°303 is a possible example of a Be/X-ray binary star. It is a periodic, radio-emitting binary system that is also the gamma-ray source, CG135+01. It is also a variable radio source characterized by periodic, non- thermal radio outbursts with a period of 26.496 d. The 26.5 d period is attributed to the eccentric orbital motion of a compact object, possibly a neutron star, around a rapidly rotating B0 Ve star.
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K Centauri is a possible binary star in the southern constellation of Centaurus. It has a white hue and is bright enough to be visible to the naked eye, having an apparent visual magnitude of +5.04. K Centauri is located at a distance of approximately 410 light years from the Sun based on parallax, and it has an absolute magnitude of −0.91. This is an ordinary A-type main- sequence star with a stellar classification of A1V.
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HD 111597 is a suspected astrometric binary star system in the southern constellation of Centaurus. It has the Bayer designation p Centauri, while HD 111597 is the star's identifier from the Henry Draper catalogue. The system is visible to the naked eye as a faint point of light with an apparent visual magnitude of 4.90. It is located at a distance of approximately 380 light years from the Sun based on parallax, and has an absolute magnitude of −0.53.
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This star, located away, is a K-type subgiant of spectral type K1. The other twelve naked-eye stars in Caelum are not referred to by Bode's Bayer designations anymore, including RV Caeli. alt=An image of the Seyfert galaxy HE0450-2958, showing the active nucleus One of the nearest stars in Caelum is the eclipsing binary star RR Caeli, at a distance of . This star system consists of a dim red dwarf and a white dwarf.
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These types of stars are a few times more massive than the Sun, and have effective temperatures of about 10,000 to 30,000 K. x1 Centauri is just over 3 times more massive than the Sun and has a temperature of about 11,300 K. The star x2 Centauri, which lies about 0.4′ away from x1 Centauri, may or may not form a physical binary star system with x1 Centauri, as the two have similar proper motions and distances.
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By 2007, the two stars were so close to merging, that its magnitude, as measured on Earth, appeared roughly spherical, leading to the loss of the second maximum immediately prior to its outburst. This evidence was the first of its kind to conclusively demonstrate that a contact binary star can end its evolution in a stellar merger and also gave scientists a framework within which to identify other stars as contact binaries and predict future mergers.
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HD 107914 is a binary star in the constellation Centaurus, with an estimated distance of from the Solar System. The primary has a stellar classification of A7-8 III, making it a giant star. Measurement of the proper motion of this system show that it has a low transverse velocity relative to the Sun. For this reason, it has been compared to the hypothetical "Nemesis" star since it may pass through the Oort cloud in the future.
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The secondary, visible in small telescopes as a star of magnitude 9.4, is a binary with two components, magnitudes 10 and 11. There is an optical companion to Iota Librae; 25 Librae is a star of magnitude 6.1, 219 light-years from Earth and visible in binoculars. Mu Librae is a binary star divisible in medium-aperture amateur telescopes, 235 light-years from Earth. The primary is of magnitude 5.7 and the secondary is of magnitude 6.8.
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Nu Piscium (ν Piscium) is an orange-hued binary star system in the zodiac constellation of Pisces. Prior to the formation of the modern constellation boundaries in 1930, it was designated 51 Ceti in the Cetus constellation. Nu Piscium is visible to the naked eye, having a combined apparent visual magnitude of 4.44. Based upon an annual parallax shift of 8.98 mas as seen from Earth, it is located about 363 light years from the Sun.
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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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In 1904, one of the discoveries made using Great Refractor of Potsdam (a double telescope with two doublets) was of the interstellar medium. The astronomer Professor Hartmann determined from observations of the binary star Mintaka in Orion, that there was the element calcium in the intervening space. ;Triplets Planet Pluto was discovered by looking at photographs (i.e. 'plates' in astronomy vernacular) in a blink comparator taken with a refracting telescope, an astrograph with a 3 element 13-inch lens.
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17 Cygni is the Flamsteed designation for a binary star system in the northern constellation of Cygnus. It has an apparent visual magnitude of 5.00, so, according to the Bortle scale, it is visible from suburban skies at night. Measurements made with the Hipparcos spacecraft show an annual parallax shift of 0.0478″, which is equivalent to a distance of around from the Sun. It has a relatively high proper motion, traversing the celestial sphere at the rate of /year.
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Delta Pyxidis (δ Pyxidis) is binary star system in southern constellation of Pyxis. Having an apparent visual magnitude of +4.877, it is bright enough to be visible to the naked eye. Based upon an annual parallax shift of 13.19 mas as seen from Earth, it is located around 250 light years from the Sun. In Chinese, (), meaning Celestial Dog, refers to an asterism consisting of δ Pyxidis, e Velorum, f Velorum, β Pyxidis, α Pyxidis and γ Pyxidis.
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Tau Draconis, Latinized from τ Draconis, is an astrometric binary star system in the northern circumpolar constellation of Draco. The star is faintly visible to the naked eye, having an apparent visual magnitude of 4.45. Based upon an annual parallax shift of 22.28 mas as measured from Earth, it is located around 146 light years from the Sun. Its proper motion is propelling it across the sky at the rate of 0.176 arc seconds per year.
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Kepler-453b is a transiting circumbinary exoplanet in the binary-star system Kepler-453. It orbits the binary system in the habitable zone every 240.5 days. The orbit of the planet is inclined relative to the binary orbit therefore precession of the orbit leads to it spending most of its time in a non-transiting configuration. By the time the TESS and PLATO spacecraft are available for follow up observations it will no longer be transiting.
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HY Velorum is a binary star system in the southern constellation of Vela. It is a dim star but visible to the naked eye with an apparent visual magnitude of 4.83. The distance to this system, as estimated from its annual parallax shift of , is 460 light years. HY Vel most likely forms a gravitationally bound pair with the magnitude 5.45 binary system KT Vel (HD 74535); both are members of the IC 2391 open cluster.
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Theta Piscis Austrini (θ Piscis Austrini) is a binary star system in the southern constellation of Piscis Austrinus. It is faintly visible to the naked eye with a combined apparent visual magnitude of +5.01. Based upon an annual parallax shift of 10.16 mas as seen from the Earth, the system is located around 320 light years from the Sun. The binary nature of this system was discovered in 1951 by South African astronomer W. S. Finsen.
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The component k1 Puppis is a binary star system in its own right, while k2 Puppis is a variable star. Each star within the k Puppis optical pair is between 450 and 470 light years from Earth. k Puppis is listed in the General Catalogue of Variable Stars as a suspected variable star, but the range and type are not stated. The International Bulletin of Variable Stars has since published research showing that k2 Puppis is the variable component.
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Taylor also made observations on the comet of 1831. Inside of the Observatory in Goldingham's time Taylor was replaced by Captain William Stephen Jacob in 1848, who continued the work on star positions. Jacob found orbital anomalies in the binary star 70 Ophiuchi that he claimed were evidence of a possible extrasolar planet. From 1859 to 1861 Major J.F. Tennant was in charge of the observatory and magnetic observations began to be made using vertical force and declination magnetometers.
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Eta Delphini, Latinized from η Delphini, is a candidate astrometric binary star system in the northern constellation of Delphinus. It has an apparent magnitude of about 5.4, meaning that it is faintly visible to the naked eye. Based upon a parallax measurement of 13.81 mas made by the Hipparcos spacecraft, this star is around 240 light years away from the Sun. It is advancing in general direction of the Earth with a radial velocity of −25 km/s.
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Delta Aurigae (δ Aur, δ Aurigae) is the Bayer designation for an astrometric binary star in the constellation Auriga. It is visible to the naked eye with an apparent visual magnitude of 3.715. Based upon its annual parallax shift of 25.88 mas, it is some distant from the Earth, give or take an eight light-year margin of error. This star is the namesake for the Delta Aurigids, a meteor shower that occurs between October 6–15.
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WW Aurigae is an eclipsing binary star system in the northern constellation of Auriga. It has a combined maximum apparent visual magnitude of 5.86, which is bright enough to be dimly visible to the naked eye. Based upon an annual parallax shift of , it is located 297 light years from the Earth. The system is moving further away with a heliocentric radial velocity of −9 km/s, having come to within some 3.12 million years ago.
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Omega Cassiopeiae (ω Cassiopeiae) is a binary star system in the northern constellation of Cassiopeia. It has a combined apparent visual magnitude of +4.99, which means it is a faint star but visible to the naked eye. Based upon an annual parallax shift of 4.65 mas as seen from Earth, this system is located roughly 700 light years from the Sun. At that distance, the visual magnitude is diminished by an extinction of 0.16 due to interstellar dust.
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29 Aquarii is a binary star system located around 590 light years away from the Sun in the equatorial constellation of Aquarius. 29 Aquarii is the Flamsteed designation; the system also bears the variable star designation DX Aquarii. It is a challenge to view with the naked eye, appearing as a dim star with a combined apparent visual magnitude of 6.39. The system is moving further from the Earth with a heliocentric radial velocity of about +15 km/s.
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71 Aquilae (abbreviated 71 Aql) is a binary star in the equatorial constellation of Aquila. 71 Aquilae is its Flamsteed designation though it also bears the Bayer designation l Aquilae. The apparent visual magnitude of the system is 4.33, making it bright enough to be viewed by the naked eye. It has an annual parallax shift of 9.67 mas, which equates to a physical distance of from Earth, give or take a 30 light-year margin of error.
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45 Aurigae or PLX 1468.2 is a binary star system in the northern constellation of Auriga. It has an apparent visual magnitude of 5.34, making it visible to the naked eye under suitable viewing conditions. An annual parallax shift of 16.89 mas as seen from Earth's orbit indicates the system is located about 193 light years from the Sun. This is a close, single-lined spectroscopic binary with a circularized orbit with a short period of 6.5 days.
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40 Aurigae is a binary star in the constellation Auriga. Its apparent magnitude is 5.345, meaning it can just barely be seen with the naked eye. Based on parallax estimates made by the Hipparcos spacecraft, the system is located some 340 light-years (104 parsecs) away. 40 Aurigae is a spectroscopic binary, meaning the two stars are too close to be individually resolved, but periodic Doppler shifts in their spectra indicate there must be orbital motion.
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39 Cygni is a binary star system near the southern border of the northern constellation of Cygnus, approximately 250 light years away from Earth. It is visible to the naked eye as an orange-hued star with an apparent visual magnitude of 4.43. The system is moving closer to the Sun with a heliocentric radial velocity of −17 km/s. This is a single-lined spectroscopic binary with an orbital period of about and an eccentricity of 0.5.
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Nu Cancri, Latinized from ν Cancri, is a binary star in the zodiac constellation of Cancer. It is faintly visible to the naked eye with an apparent visual magnitude of +5.46. Based upon an annual parallax shift of 8.31 mas as seen from the Earth, the star is located roughly 390 light years from the Sun. This is a single-lined spectroscopic binary system with an orbital period of 3.8 years and an eccentricity of 0.35.
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10 Boötis is a suspected astrometric binary star system in the northern constellation of Boötes, located around 528 light years away from the Sun. It is visible to the naked eye under suitable viewing conditions as a dim, white- hued star with an apparent visual magnitude of 5.76. Its magnitude is diminished by an extinction of 0.17 due to interstellar dust. This system is moving away from the Earth with a heliocentric radial velocity of +6 km/s.
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15 Boötis is a binary star system in the northern constellation of Boötes, located approximately 260 light years away from the Sun. It is visible to the naked eye as a dim, orange-hued star with an apparent visual magnitude of 5.45. The system has a relatively high proper motion, traversing the celestial sphere at the rate of 0.166 arc seconds per annum. It is moving away from the Earth with a heliocentric radial velocity of +16.8 km/s.
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In 1975, Yasuho Yamashita noted that some higher temperature carbon stars displayed the typical spectral characteristics of a CH star, but did not have the same kinematic properties. That is, they did not have the higher space velocities characteristic of the older stellar population. These were dubbed CH-like stars. Many CH stars are known to be members of binary star systems, and it is reasonable to believe this is (or was) the case for all CH stars.
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This is a single-lined spectroscopic binary star system with an orbital period of 207.357 days and an eccentricity of 0.55. The primary component has the spectrum of an evolved F-type giant/bright giant hybrid with a stellar classification of F7 II/III. It is around 46 million years old with 6.9 times the mass of the Sun. The star is radiating 3,919 times the Sun's luminosity from its photosphere at an effective temperature of 6,495 K.
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Delta Sagittae (Delta Sge, δ Sagittae, δ Sge) is a binary star in the constellation of Sagitta, with an apparent magnitude of +3.68. The primary component is a red M-type bright giant, and the secondary is a B-type main- sequence star. It is approximately 430 light years from Earth, based on its Gaia Data Release 2 parallax. Delta Sagittae is a spectroscopic binary with a composite spectrum, meaning that light from both stars can be detected.
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WD 0137-349 is a binary star in the constellation of Sculptor. It is located about 330 light-years (100 parsecs) away, and appears exceedingly faint with an apparent magnitude of 15.33. It is composed of a white dwarf and a brown dwarf in orbit around it, and it one of the few systems to a white dwarf and an associated brown dwarf. The brown dwarf orbits with a period of 116 minutes, or nearly 2 hours.
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Chi Geminorum (χ Gem) is a binary star system in the constellation Gemini, near the western border with Cancer. It can be viewed with the naked eye on a dark night, having an apparent visual magnitude of 4.98. Based upon an annual parallax shift of 12.73 mas, it is located roughly 260 light years from the Sun. The two components of this system form a spectroscopic binary with an orbital period of 2,437.8 days and an eccentricity of 0.06.
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Sigma Aquilae, Latinized from σ Aquilae, is the Bayer designation for a binary star system in the equatorial constellation of Aquila. The baseline apparent magnitude of the pair is +5.17, which, according to the Bortle Dark-Sky Scale, is bright enough to be seen with the naked eye from suburban skies. Because of the Earth's orbit about the Sun, this system has an annual parallax shift of 4.18 mas. This provides a distance estimate of approximately .
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Xi Arietis, Latinized from ξ Arietis, is the Bayer designation for a binary star system in the northern constellation of Aries. It has an apparent visual magnitude of 5.46, and so is dimly visible to the naked eye. Based upon an annual parallax shift of as seen from Earth, it is distant from the Sun. At that distance, the visual magnitude of the star is diminished by an extinction factor of 0.24 due to interstellar dust.
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23 Ursae Majoris, or 23 UMa, is a binary star system in the constellation Ursa Major, located is approximately 77.7 light years from the Sun. It has the Bayer designation h Ursae Majoris; 23 Ursae Majoris is the Flamsteed designation. The system is visible to the naked eye as a yellow-white hued star with an apparent visual magnitude of +3.65. It is moving closer to the Earth with a heliocentric radial velocity of −10 km/s.
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HR 3643 is a binary star system in the southern constellation of Carina. It has the Bayer designation G Carinae, with HR 3643 being the star's designation in the Bright Star Catalogue. The system is visible to the naked eye with an apparent visual magnitude of 4.48. It is located at a distance of approximately 401 light years from the Sun based on parallax, and is drifting further away with a radial velocity of +22.5 km/s.
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At the time, the fused quartz gyroscopes created for Gravity Probe B were the most nearly perfect spheres ever created by humans. The gyroscopes differ from a perfect sphere by no more than 40 atoms of thickness. One is pictured here refracting the image of Albert Einstein in background. thumb The Gravity Probe B experiment comprised four London moment gyroscopes and a reference telescope sighted on HR8703 (also known as IM Pegasi), a binary star in the constellation Pegasus.
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Delta1 Gruis, Latinized from δ1 Gruis, is a candidate binary star system in the constellation Grus. With a peak apparent visual magnitude of 3.97, it is bright enough to be seen with the naked eye at night. The distance to this system, as determined using an annual parallax shift of 10.54 mas as seen from the Earth, is around 309 light years. It is gradually moving away from the Sun with a radial velocity of +4.9 km/s.
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HD 34790 is a double-lined spectroscopic binary star system in the northern constellation of Auriga. It has a combined apparent magnitude of 5.66, which means it is faintly visible to the naked eye. Based upon observations by the Hipparcos satellite, it is located around 289 light years away. It has a combined stellar classification of A1Vs, matching that of an A-type main sequence star, and shines with 35 times the luminosity of the Sun.
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It forms a triangle with the fainter φ1 Hydrae and φ2 Hydrae, between μ Hydrae and ν Hydrae. This is a single-lined spectroscopic binary star system with an orbital period of about 1,200 days and an eccentricity of 0.1. The primary, component A, is an evolved G-type giant star with a stellar classification of G8 III. It is a red clump star, which means it is generating energy through the fusion of helium at its core.
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Kappa Cephei, Latinized from κ Cephei, is a binary star system in the northern circumpolar constellation of Cepheus. It is visible to the naked eye as a faint, blue white-hued point of light with an apparent visual magnitude is 4.39. The system is located approximately 323–326 light years distant from the Sun, based on parallax. The two gravitationally-bound members of this system had an angular separation of along a position angle of 120°, as of 2015.
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In astronomy, Gaia16aye is a gravitational microlensing event of the star 2MASS 19400112+3007533 (the source star) by a dimmer binary star system (the lens star system). The source star 2MASS 19400112+3007533 is a magnitude 14.5 (Gaia RP) star in Cygnus. It was closely observed during a set of brightening events caused by gravitational microlensing in 2016. The Gaia16aye event was first noticed by the Gaia space mission via an alert on August 9, 2016.
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Like most halo stars, it has a low abundance of elements other than hydrogen and helium—what astronomers term a metal-poor star. Once suspected of being a binary star with a period of 175 days, current consensus is that it is single. Previous suspected observations of a stellar companion were probably "superflares"—analogous to the Sun's solar flares, but hundreds to millions of times more energetic. It had one of the first nine identified superflares.
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CE Gruis (previously called Grus V-1) is a faint binary star system in the constellation Grus. Its brightness changes between magnitudes 17.4 and 19.5 with a period of 108.6 minutes. It is composed of a white dwarf and donor star, locked into a synchronous orbit. In such systems, known as polars, material from the donor star does not form an accretion disc around the white dwarf because of its intense magnetic field, but rather streams directly onto it.
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Delta Muscae, Latinized from δ Muscae, often catalogued as HD 112985, is a spectroscopic binary star system and the closest to the Earth in the southern hemisphere constellation of Musca (the Fly) at a distance of approximately 27.8 parsecs (91.0 light years). The main star is classified as a giant star with an orange tint. It is one of the stars given a Bayer designation by astronomer Johann Bayer. It was recorded in Bayer's 1603 publication Uranometria.
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Photograph of Lacerta 2 Lacertae is a binary star in the constellation of Lacerta. With an apparent magnitude of about 4.5, it is faintly visible to the naked eye. Its parallax, measured by the Hipparcos spacecraft, is 5.88 milliarcseconds, corresponding to a distance of about 550 light years (170 parsecs). It is projected against the Lacertae OB1 stellar association to the northeast of the main concentration of stars, but it is likely to be a foreground object.
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Glycolaldehyde has been identified in gas and dust near the center of the Milky Way galaxy, in a star-forming region 26000 light-years from Earth, and around a protostellar binary star, IRAS 16293-2422, 400 light years from Earth. Observation of in- falling glycolaldehyde spectra 60 AU from IRAS 16293-2422 suggests that complex organic molecules may form in stellar systems prior to the formation of planets, eventually arriving on young planets early in their formation.
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HR 1884 is a spectroscopic binary star in the constellation Auriga. The primary is a G type supergiant star while the secondary is probably a B type main sequence star. The possible spectroscopic binary nature of the star was first noted in 1983 by Gilbert Burki and Michel Mayor in a paper on the rate of binaries among supergiant stars. In the same year, William P. Bidelman noted that the stellar spectrum was composite indicating a companion star.
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32 Cygni 32 Cygni (32 Cyg, Omicron2 Cyg, ο2 Cyg) is the Flamsteed designation for a binary star system in the Cygnus constellation. It is a 4th magnitude star, which can be seen with the naked eye under suitably dark skies. Parallax measurements give an estimated distance of 1,100 light-years (320 parsecs) from the Earth. However, Schröder et al. (2007) suggest the actual value, after correcting for Malmquist bias, may be closer to 1,174 light-years (360 parsecs).
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53 Eridani (abbreviated 53 Eri), also designated l Eridani (l Eri), is a binary star in the constellation of Eridanus. The system has a combined apparent magnitude of 3.87, making it visible to the naked eye even in inner city skies. Parallax estimates made by the Hipparcos spacecraft put it at a distance of about 110 light-years, or 33.7 parsecs, from the Sun. The two components are designated 53 Eridani A (officially named Sceptrum) and B.
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This is an Algol-like eclipsing binary star system, with a period of 2.3274 days and an eccentricity of 0.07. Its apparent magnitude varies from 4.91m to 5.9m. The secondary is filling its roche lobe and there is evidence of large-scale mass transfer in the past, with the star being more evolved than the primary. Along with λ Tau, it was one of the first stars on which rotational line broadening was observed, by Frank Schlesinger in 1911.
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Founded in the mid-'90s, the Massive Monkees have 25 active members including former Binary Star rapper One Be Lo, who performs as the MC at their shows. The crew was created through the merger of the Massive Crew and the Universal Style Monkees. Massive Monkees' style is viewed as that of fundamental B-boys/B-girls. Additionally, Massive Monkees performs at high schools to diffuse the notion that hip-hop and gangs go hand- in-hand.
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HD 212301 is a binary star system in the south circumpolar constellation of Octans. This star is also called HIP 110852. With an apparent visual magnitude of 7.76, it is too faint to be visible to the naked eye. The system is located at a distance of 177 light years from the Sun based on parallax, and is drifting further away with a radial velocity of +4.7 km/s. It has an absolute magnitude of 4.06.
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Omicron Lupi (ο Lup) is a binary star in the southern constellation of Lupus. It is a visible to the naked eye with a combined apparent visual magnitude of 4.323. Based upon an annual parallax shift of 8.07 mas as seen from Earth, it is located around 400 light years from the Sun, give or take 30 light years. At that distance, the visual magnitude of the system is diminished by an extinction factor of due to interstellar dust.
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The constellation Virgo as it appears in the manga. The series is named after Spica, a binary star system in the constellation Virgo and one of the brightest stars in the nighttime sky. It appears as one star because of the relatively low center-to-center distance between the two component stars, estimated at an average of 11 million miles (17.7 million km). Astronomical observations also suggest that there may be additional stars in the Spica system.
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HD 134687 (e Lupi) is a binary star system in the southern constellation Lupus. It is visible to the naked eye with an apparent visual magnitude of 4.81. The distance to HD 134687 can be estimated from its annual parallax shift of , yielding a separation of roughly 730 light years. It is a member of the ~11 million year old Upper Centaurus Lupus subgroup of the Scorpius–Centaurus Association, the closest OB association to the Sun.
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Omega Herculis (ω Herculis, abbreviated Ome Her, ω Her) is a binary star system in the northern constellation of Hercules. Based upon an annual parallax shift of 13.04 mas as seen from Earth, it is located around 250 light-years from the Sun. It is faintly visible to the naked eye, having a combined apparent visual magnitude of 4.58. The system is a candidate for membership in the Ursa Major Moving Group, although this remains uncertain.
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Delta Cassiopeiae (δ Cassiopeiae, abbreviated Delta Cas, δ Cas) is an eclipsing binary star system in the northern circumpolar constellation of Cassiopeia. Based on parallax measurements taken during the Hipparcos mission, it is approximately from the Earth. Delta Cassiopeiae is the primary or 'A' component of a multiple star system designated WDS J01258+6014. Delta Cassiopeiae's two components are therefore designated WDS J01258+6014 Aa and Ab. Aa is officially named Ruchbah , the traditional name for the system.
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Zeta Capricorni, Latinized from ζ Capricorni, is a fourth-magnitude star in the constellation Capricornus. ζ Capricorni is a binary star, with the primary component ζ Capricorni A being a yellow G-type giant with an apparent magnitude of +3.77. It is considered one of the prototypical examples of a Barium star, properties of which include overabundances of carbon molecules (such as C2) and s-process elements. Zeta Capricorni has an overabundance of the s-process element praseodymium.
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4 Camelopardalis is a binary star in the northern constellation of Camelopardalis, located 179 light years away from the Sun, based upon parallax. With a combined apparent visual magnitude of 5.29, it is visible to the naked eye as a faint, white-hued star. The pair have a relatively high proper motion, traversing the celestial sphere at an angular rate of per year. The system's proper motion makes it a candidate for membership in the IC 2391 supercluster.
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This is a spectroscopic binary star system with components that orbit each other every 3848.8 days (10.5 years). The combined stellar classification of the system is K0.5 IIIb, which matches the spectrum of a normal luminosity giant star. It has an apparent visual magnitude of 2.4, so it is somewhat outshined by its first magnitude neighbors Achernar (α Eridani) and Fomalhaut (α Piscis Australis). Based upon parallax measurements, this system is at a distance of about from the Earth.
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HD 177830 is a 7th magnitude binary star system located approximately 205 light-years away in the constellation of Lyra. The primary star is slightly more massive than our Sun, but cooler being a type K star. Therefore, it is a subgiant clearly more evolved than the Sun. In visual light it is four times brighter than the Sun, but because of its distance, about 205 light years, it is not visible to the unaided eye.
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QS Telescopii is a faint binary star system in the constellation Telescopium. It is composed of a white dwarf and main sequence donor star, in this case the two are so close and fused into orbit facing one another. Known as polars, material from the donor star does not form an accretion disk around the white dwarf, but rather streams directly onto it. This is due to the presence of the white dwarf's strong magnetic field.
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75 Cancri (abbreviated to 75 Cnc) is a binary star in the constellation of Cancer. The system is located about 102 light-years (31 parsecs) away, based on its stellar properties. 75 Cancri is a spectroscopic binary, which means the two stellar components are too close to be resolved, but periodic Doppler shifts in their spectra indicate orbital motion. In this case, light from both stars can be detected, and it is a double-lined spectroscopic binary.
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HD 91190 is a suspected astrometric binary star system in the northern circumpolar constellation of Draco. It is faintly visible to the naked eye, having an apparent visual magnitude of 4.86. The distance to HD 91190, as estimated from its annual parallax shift of , is around 720 light years. This system is moving further away from the Sun with a heliocentric radial velocity of +17 km/s, having come to within some 2.4 million years ago.
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6 Draconis is a single-lined spectroscopic binary star system in the northern constellation of Draco, located about 430 light years away from the Sun. It is visible to the naked eye as an orange-hued star with an apparent visual magnitude of 4.95. The system is moving further from the Earth with a heliocentric radial velocity of 3 km/s. The variable radial velocity of this star system was announced by W. W. Campbell in 1922.
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27 Canis Majoris is a binary star system in the northern constellation of Canis Major, located approximately 1,700 light years away from the Sun. It has the variable star designation EW Canis Majoris; 27 Canis Majoris is the Flamsteed designation. This system is visible to the naked eye as a dim, blue- white hued star with an apparent visual magnitude of +4.65. It is moving away from the Earth with a heliocentric radial velocity of 16 km/s.
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This spectroscopic binary star system has an orbital period of 389.31 days, a semimajor axis of 1.48 AU, and an eccentricity of 0.2586. Their variable radial velocity was discovered by H. M. Reese in 1902 at Lick Observatory. Both components are evolved, K-type giant stars, most likely on their first ascent along the red giant branch. The primary, component A, has a stellar classification of K4 III while the secondary, component B, may be K1: III.
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Tau Coronae Borealis, Latinized from τ Coronae Borealis, is a possible astrometric and spectroscopic binary star system in the northern constellation of Corona Borealis. It is visible to the naked eye with an apparent visual magnitude of 4.76. Tau CrB has a visible companion of visual magnitude 13.2 and they have been treated as a common proper motion pair. As of 2014, the pair had an angular separation of 2.20 arc seconds along a position angle of 186°.
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Iota Coronae Borealis, Latinized from ι Coronae Borealis, is a binary star system in the constellation Corona Borealis. It is visible to the naked eye with a combined apparent visual magnitude of is 4.96. Based upon an annual parallax shift of 10.46 mas as seen from the Earth, it is located about 312 light years from the Sun. This is a single-lined spectroscopic binary with an orbital period of 35.5 days and an eccentricity of 0.56.
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Theta Coronae Borealis, Latinized from θ Coronae Borealis, is a binary star system in the constellation Corona Borealis. It shines with a combined apparent visual magnitude (V band) of 4.13. There are two components: Theta Coronae Borealis A is of apparent magnitude 4.16, while Theta Coronae Borealis B lies around 1 arcsecond distant and has an apparent magnitude of 6.29. The system is located around 375 light-years from Earth, as estimated from its parallax of 8.69 milliarcseconds.
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Kappa1 Sculptoris is a binary star system in the southern constellation of Sculptor. It is faintly visible to the naked eye, with a combined apparent visual magnitude of +5.51. Based upon an annual parallax shift of 12.91 mas as measured from Earth, it is located roughly 250 light years from the Sun. The pair orbit each other with an estimated period of 616 years, a semimajor axis of 1.5 arc seconds, and an eccentricity of 0.1.
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Some are available as add-ons. Although objects that form part of a planetary system move, and stars rotate about their axes and orbit each other in multiple star systems, stellar proper motion is not simulated, and galaxies are at fixed locations. As a result, the constellations in Celestia do not gradually change shape as they do in the real world. In addition, Celestia's binary star catalogs only describe a few hundred systems of multiple stars.
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23 Comae Berenices is a binary star system in the northern constellation of Coma Berenices, situated a few degrees away from the North Galactic Pole. It is visible to the naked eye as a faint, white-hued point of light with an apparent visual magnitude of 4.80. The system is located around 310 light years away from the Sun, based on parallax. It is moving closer to the Earth with a heliocentric radial velocity of −16 km/s.
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HR 8442 is a spectroscopic binary star in the constellation Cepheus. The primary is a G type giant star while the secondary's spectral type is unknown. The spectroscopic binary nature of the star was first noticed by Jose Renan de Medeiros and Michel Mayor using radial velocity measurements from the Coravel spectrometer at Haute-Provence Observatory. Roger griffin then placed the star on his observing program at Cambridge Observatory leading to an orbital solution being published in 2015.
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Upsilon Lupi, Latinized from υ Lupi, is a star system in the southern constellation of Lupus. It is faintly visible to the naked eye with an apparent visual magnitude of 5.37. Based upon an annual parallax shift of 8.02 mas as seen from Earth, it is located around 410 light years from the Sun. The two components of Upsilon Lupi share a common proper motion through space and most likely form a wide binary star system.
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Epsilon Carinae (ε Carinae, abbreviated Epsilon Car, ε Car), officially named Avior , is a binary star in the southern constellation of Carina. At apparent magnitude +1.86 it is one of the brightest stars in the night sky, but is not visible from the northern hemisphere. The False Cross is an asterism formed of Delta Velorum, Kappa Velorum, Iota Carinae and ε Carinae. It is so called because it is sometimes mistaken for the Southern Cross, causing errors in astronavigation.
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Rho Tucanae (ρ Tuc, ρ Tucanae) is a binary star system in the southern constellation of Tucana. It is visible to the naked eye with a combined apparent visual magnitude of +5.38. Based upon an annual parallax shift of 24.37 mas as seen from Earth, it is located 131 light years from the Sun. This is a single-lined spectroscopic binary with a close, nearly circular orbit having a period of 4.82 days and an eccentricity of 0.02.
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Zeta Horologii, Latinized from ζ Horologii, is a yellow-white hued binary star system in the southern constellation of Horologium. It is visible to the naked eye with a combined apparent visual magnitude of 5.20. Based upon an annual parallax shift of 20.37 mas as seen from Earth, it is located around 160 light years from the Sun. This system was determined to be a double-lined spectroscopic binary by J. H. Moore in 1911−12.
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HD 80606 and HD 80607 are two stars comprising a binary star system. They are approximately 217 light-years away in the constellation of Ursa Major. Both stars orbit each other at an average distance of 1,200 astronomical units. The binary system is listed as Σ1341 in the Struve Catalogue of Double Stars, however this designation is not in wide use and the system is usually referred to by the HD designations of its constituent stars.
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The minimum stable star to circumbinary planet separation is about 2–4 times the binary star separation, or orbital period about 3–8 times the binary period. The innermost planets in all the Kepler circumbinary systems have been found orbiting close to this radius. The planets have semi-major axes that lie between 1.09 and 1.46 times this critical radius. The reason could be that migration might become inefficient near the critical radius, leaving planets just outside this radius.
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HR 6384 is a binary star system in the southern constellation of Ara, the Altar. The system is faintly visible to the naked eye with a combined apparent visual magnitude that fluctuates around 6.153, and it is located at a distance of approximately from the Sun. It is drifting closer with a radial velocity of around −34 km/s. The system appears to be a close, interacting binary with a hot secondary component of class A or hotter.
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Chandra observations have also revealed a point source at the position of the central star. The spectrum of this source extends to the hard part of the X-ray spectrum, to 0.5–. A star with the photospheric temperature of about would not be expected to emit strongly in hard X-rays, and so their presence is something of a mystery. It may suggest the presence of a high temperature accretion disk within a binary star system.
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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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Gamma Camelopardalis, Latinized from γ Camelopardalis, is a suspected wide binary star system in the northern circumpolar constellation of Camelopardalis. With a visual magnitude of 4.66, it is faintly visible to the naked eye. Based upon an annual parallax shift of 9.09 mas as seen from Earth, this star is located about 359 light years from the Sun. The brighter primary, designated component A, is a white-hued A-type subgiant star with a stellar classification of A2 IVn.
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Omega Sagittarii, which is Latinized from ω Sagittarii, is a binary star system in the constellation of Sagittarius, near the eastern constellation border with Capricornus. It is formally named Terebellum . This system has a yellow hue and is faintly visible to the naked eye with an apparent visual magnitude of 4.70. It is located at a distance of 76 light years away from the Sun based on parallax, and is drifting closer with a radial velocity of −16 km/s.
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As of 2003, Achernar is the least spherical star in the Milky Way studied to date. It spins so rapidly that it has assumed the shape of an oblate spheroid with an equatorial diameter 56% greater than its polar diameter. The polar axis is inclined about 65° to the line of sight from the Earth. Since it is actually a binary star, its highly distorted shape may cause non-negligible departures of the companion's orbital trajectory with respect to a Keplerian ellipse.
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In 2018 Haswell was part of the team that was first to identify a planet around Barnard's Star, the closest single (non-binary) star to Earth, a red dwarf star that is six light years away from Earth. Using the radial velocity method, the team discovered Barnard's Star b. The solar system around Barnard's Star touches on the edge of the Oort cloud. Barnard's Star b has a mass three times that of Earth and orbits Barnard's Star in 233 days.
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Regulus is a multiple star system consisting of at least four stars. Regulus A is the dominant star, with a binary companion 177" distant that is thought to be physically related. Regulus D is a 12th magnitude companion at 212", but is an unrelated background object. Regulus A is a binary star consisting of a blue-white main sequence star of spectral type B7V, which is orbited by a star of at least 0.3 solar masses, which is probably a white dwarf.
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2 Persei is a binary star system in the northern constellation Perseus, located around 500 light years away from the Sun. It is visible to the naked eye as a faint, blue-white hued star with an apparent visual magnitude is 5.70. The system is moving further away from the Earth with a heliocentric radial velocity of 11 km/s. In 1970 radial velocity measurements from spectrograms taken at David Dunlap Observatory indicated it was a single-lined spectroscopic binary.
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Xi Orionis (ξ Orionis) is a binary star system in the northeastern part of the constellation of Orion, well above the red giant star, Betelgeuse in the sky. It lies next to another blue main-sequence star, Nu Orionis which is somewhat closer at 520 light years. The apparent visual magnitude of Xi Orionis is 4.47, which is bright enough to be seen with the naked eye. The distance to this star, as determined using the parallax method, is roughly 610 light years.
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Mu Velorum (μ Vel, μ Velorum) is a binary star system in the southern constellation Vela. The two stars orbit each other with a semi-major axis of 1.437 arcseconds and a period of 116.24 years. (Wulff-Dieter Heintz (1986) lists a period of 138 years with his orbital elements.) The pair have a combined apparent visual magnitude of 2.69, making the system readily visible to the naked eye. From parallax measurements, the distance to this system is estimated to be .
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HD 10307 (HR 483) is a spectroscopic binary star in the constellation Andromeda. The primary is similar to the Sun in mass, temperature and metal content. situated about 42 light-years from Earth Its companion, HR 483 B, is a little-studied red dwarf. HD 10307 was identified in September 2003 by astrobiologist Margaret Turnbull from the University of Arizona in Tucson as one of the most promising nearby candidates for hosting life based on her analysis of the HabCat list of stars.
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HR 4072 is a binary star system in the northern circumpolar constellation of Ursa Major. It has the variable star designation ET Ursae Majoris, abbreviated ET Uma, while HR 4072 is the system's designation from the Bright Star Catalogue. It has a white hue and is faintly visible to the naked eye with an apparent visual magnitude that fluctuates around 4.94. The system is located at a distance of approximately 339 light years from the Sun based on parallax measurements.
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It is around five times as massive as our Sun. Beta Muscae is a binary star system around 341 light-years distant that is composed of two blue-white main-sequence stars of spectral types B2V and B3V that orbit each other every 194 years. They are eight and six times as massive as the Sun, respectively, and have about 3.5 times its diameter. Zeta2 Muscae is a white main sequence star of spectral type A5V around 330 light- years distant from Earth.
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There are 37 stars brighter than apparent magnitude 6.5 in the constellation; three are brighter than magnitude 4.5. 46 Leonis Minoris, an orange giant of magnitude 3.8, is located some 95 light-years from Earth. At magnitude 4.4, Beta Leonis Minoris is the second-brightest star and the only one in the constellation with a Bayer designation. It is a binary star, the brighter component of which is an orange giant and the fainter a yellow-white main sequence star.
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Its traditional name means "breast" and refers to its position in the constellation. Delta Cygni (the proper name is Fawaris) is another bright binary star in Cygnus, 171 light-years with a period of 800 years. The primary is a blue-white hued giant star of magnitude 2.9, and the secondary is a star of magnitude 6.6. The two components are visible in a medium-sized amateur telescope. The fifth star in Cygnus above magnitude 3 is Aljanah, designated Epsilon Cygni.
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Diagram of an intermediate polar. Matter flows from the companion star into an accretion disk around the white dwarf, but is disrupted by the white dwarf's magnetic field. An Intermediate Polar (also called a DQ Herculis Star) is a type of cataclysmic variable binary star system with a white dwarf and a cool main-sequence secondary star. In most cataclysmic variables, matter from the companion star is gravitationally stripped by the compact star and forms an accretion disk around it.
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Eta1 Coronae Australis, Latinized from η1 CrA, is a suspected astrometric binary star system in the constellation of Corona Australis. It is visible to the naked eye as a dim, white-hued point of light with an apparent visual magnitude of 5.456. Parallax measurements put it at a distance of 317 light- years away from the Sun. The visible component is an A-type main-sequence star with a stellar classification of A3V, which indicates it is generating energy through core hydrogen fusion.
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Gamma Librae is called Zubenelakrab, which means "the scorpion's claw", completing the suite of names referring to Libra's archaic status. It is an orange giant of magnitude 3.9, 152 light-years from Earth. Iota Librae is a complex multiple star, 377 light-years from Earth, with both optical and true binary components. The primary appears as a blue-white star of magnitude 4.5; it is a binary star indivisible in even the largest amateur instruments with a period of 23 years.
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72 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 a combined apparent visual magnitude of 4.97. The system is located approximately 550 light years away from the Sun, based on parallax, but is drifting closer with a radial velocity of −25 km/s. This is a visual binary with an orbital period of roughly 492 years and an eccentricity of 0.32.
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Omega Ursae Majoris (Omega UMa, ω Ursae Majoris, ω UMa) is the Bayer designation for a binary star system in the northern circumpolar constellation of Ursa Major. It is visible to the naked eye with an apparent visual magnitude of 4.61. Based upon an annual parallax shift of 13.24 mas, it is roughly 246 light years from the Sun. At that distance, the visual magnitude of the star is diminished by an extinction factor of 0.11 due to interstellar dust.
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19 Puppis is a binary star system in the southern constellation of Puppis, near the northern border with Hydra and Monoceros. It is visible to the naked eye as a faint, yellow-hued star with an apparent visual magnitude of 4.72. The system is located approximately 177 light years away from the system based on parallax. It is receding from the Earth with a heliocentric radial velocity of +36 km/s, having come to within some 1.4 million years ago.
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HD 2638 is a binary star system in the equatorial constellation of Cetus. The pair have an angular separation of along a position angle of 166.7°, as of 2015. This is system too faint to be visible to the naked eye, having a combined apparent visual magnitude of 9.44; a small telescope is required. The distance to this system is 179.5 light years based on parallax, and it is drifting further away with a radial velocity of +9.6 km/s.
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This is a single-lined spectroscopic binary star system with an orbital period of 36.5 days and an eccentricity of roughly 0.3. The visible component is a B-type main-sequence star with a stellar classification of B7 V. It is spinning rapidly with a projected rotational velocity of 212 km/s. The star has 4.2 times the mass of the Sun and is radiating around 611 times the Sun's luminosity from its photosphere at an effective temperature of 9,908 K.
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4 Equulei is a binary star system in the constellation of Equuleus, located about 3° to the east of Alpha Equulei. With an apparent visual magnitude of 5.94, it is just barely visible to the naked eye under good seeing conditions. The system shows an annual parallax shift of 20.44 mas as measured from Earth's orbit, which yields a distance estimate of about 160 light years. It is moving closer to the Sun with a radial velocity of −13 km/s.
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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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HR 4796 is a binary star system in the southern constellation of Centaurus. Parallax measurements put it at a distance of from the Earth. The two components of this system have an angular separation of 7.7 arcseconds, which, at their estimated distance, is equivalent to a projected separation of about 560 Astronomical Units (AU), or 560 times the separation of the Earth from the Sun. The star and its ring resemble an eye, and it is sometimes known by the nickname "Sauron's Eye".
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V1472 Aquilae is a semi-regular pulsating star in the constellation Aquila. It is actually a binary star system, the main component being a red giant of spectral type M2.5 III. Original calculations using hipparcos data gave a parallax of 7.92 ± 1.07 milliarcseconds, but reprocessing to allow for orbital motion adjusts the parallax to 2.4 ± 1.0 milliarcseconds—tripling the system's distance from Earth. The main star has a diameter 104 ± 56 times and luminosity 1100 times that of the Sun.
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18 Vulpeculae is a binary star system in the northern constellation of Vulpecula, located about 489 light years away from the Sun. It is visible to the naked eye as a faint, white-hued star with a combined apparent visual magnitude of 5.51. The system is moving closer to the Earth with a heliocentric radial velocity of −11.7 km/s. This is a double-lined spectroscopic binary system with an orbital period of 9.3 days and a small eccentricity of 0.0116.
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Nu Cygni, Latinized from ν Cygni, is a binary star system in the constellation Cygnus. Its apparent magnitude is 3.94 and it is approximately 374 light years away based on parallax. The brighter component is a magnitude 4.07 A-type giant star with a stellar classification of A0III n, where the 'n' indicates broad "nebulous" absorption lines due to rapid rotation. This white-hued star has an estimated 3.6 times the mass of the Sun and about 1.9 times the Sun's radius.
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41 Ophiuchi is a binary star system in the zodiac constellation of Ophiuchus, and is positioned less than half a degree to the south of the celestial equator. It is visible to the naked eye as a faint, orange-hued point of light with a combined apparent visual magnitude of 4.72. The distance to this system is approximately 202 light years based on parallax. This is a visual binary with an orbital period of 141 years and an eccentricity of 0.866.
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HD 1237 is a binary star system approximately 57 light-years away in the constellation of Hydrus (the Water Snake). The visible star in the system, A, is considered to be a solar analog due close mass to the sun. HD 1237 differs from the sun in that HD 1237 is much younger, has high metallicity, has much cooler temperature and is in a binary system. As of 2000, it has been confirmed that an extrasolar planet orbits the star.
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In each period of 75 days it has two maxima and two minima. AC Her is also a binary star, although the secondary can only be detected by its effect on the radial velocity of the primary. The invisible secondary is more massive than the supergiant primary, so the primary moves at relatively high velocity in its three years and three months orbit. The two stars are also surrounded by a dusty disc filling the region between 34 and 200 astronomical units (AU).
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54 Aurigae is a binary star system located around 800 light years away from the Sun in the northern constellation of Auriga. It is visible to the naked eye as a dim, blue-white hued star with a combined apparent visual magnitude of 6.02. The system is moving further from the Sun with a heliocentric radial velocity of around +19 km/s. The primary component is a B-type giant star of visual magnitude 6.22 with a stellar classification of B7 III.
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4 Cassiopeiae is a wide binary star system in the northern constellation of Cassiopeia, located approximately 790 light-years away from the Sun. It is visible to the naked eye as a faint, red-hued star with a baseline apparent visual magnitude of 4.96. At the distance of this system, its visual magnitude is diminished by an extinction of 0.56 due to interstellar dust. This system is moving closer to the Earth with a heliocentric radial velocity of −39 km/s.
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Illustration of Mu1,2 Boötis μ1 Boötis is a yellow-white F-type subgiant with an apparent magnitude of +4.31. Separated from its brighter companion by 108 arcseconds in the sky is the binary star μ2 Boötis, which has a combined spectral type of G1V and a combined brightness of +6.51 magnitudes. The components of μ2 Boötis have apparent magnitudes of +7.2 and +7.8 and are separated by 2.2 arcseconds. They complete one orbit about their common centre of mass every 260 years.
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65 Aurigae is a binary star system located 252 light years away from the Sun in the northern constellation of Auriga. It is visible to the naked eye as a faint, orange hued star with an apparent visual magnitude of 5.12. The primary, designated component A, is an aging giant star with a stellar classification of K0 III. It is 3.31 billion years old and has expanded to 13 times the Sun's radius after exhausting the hydrogen at its core.
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31 Arietis (abbreviated 31 Ari) is a binary star in the northern constellation of Aries. 31 Arietis is the Flamsteed designation. The two members of this system orbit each other with a period of 3.80 years and an eccentricity of 0.017. Both components of the system are F-type main sequence stars with a stellar classification of F7 V. The pair have an apparent visual magnitude of 5.75, which is just bright enough to be faintly visible to the naked eye.
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The system is moving further from the Earth with a heliocentric radial velocity of +1.1 km/s. The magnitude 5.88 primary, component A, is itself a binary star with a separation of – and an orbital period of around . The brighter member of this duo is a G-type bright giant with a stellar classification of G4 II and 2.6 times the mass of the Sun. Its companion is an early A-type star with double the mass of the Sun.
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53 Aquarii (abbreviated 53 Aqr) is a binary star system in the equatorial constellation of Aquarius. 53 Aquarii is its Flamsteed designation though the star also bears the Bayer designation of f Aquarii. The combined apparent visual magnitude of the pair is a 5.56, making it just visible to the naked eye in dark suburban skies. Based upon an annual parallax shift of 49.50 milliarcseconds for the first component, this system is located at a distance of approximately from Earth.
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14 Boötis is a possible binary star system located 110 light years away from the Sun in the northern constellation of Boötes. It is visible to the naked eye as a dim, yellow-white hued star with a combined apparent visual magnitude of 5.53. This system is moving closer to the Earth with a heliocentric radial velocity of −40 km/s. It has a relatively high proper motion, traversing the celestial sphere at the rate of 0.260 arc seconds per annum.
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Xi Cassiopeiae (ξ Cassiopeiae) is a blue-white hued binary star system in the northern constellation of Cassiopeia. It has an apparent visual magnitude of +4.81 and thus is faintly visible to the naked eye. Based upon an annual parallax shift of 2.28 mas as seen from Earth, this system is located roughly 1,400 light years from the Sun. At that distance, the visual magnitude of the system is diminished by an extinction factor of 0.20 due to interstellar dust.
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Nu Centauri (ν Cen, ν Centauri) is a binary star system in the southern constellation of Centaurus. The combined apparent visual magnitude of the pair is +3.41, making this one of the brightest members of the constellation. Based upon parallax measurements made during the Hipparcos mission, this star system is located at a distance of roughly from Earth. The margin of error for this distance is about 2%, which is enough to give an error in distance of ±10 light years.
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IK Pegasi (or HR 8210) is a binary star system in the constellation Pegasus. It is just luminous enough to be seen with the unaided eye, at a distance of about 154 light years from the Solar System. The primary (IK Pegasi A) is an A-type main-sequence star that displays minor pulsations in luminosity. It is categorized as a Delta Scuti variable star and it has a periodic cycle of luminosity variation that repeats itself about 22.9 times per day.
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31 Orionis is a binary star system in the equatorial constellation of Orion, located near the bright star Mintaka. It is visible to the naked eye as a faint, orange-hued point of light with a baseline apparent visual magnitude of 4.71. The distance to this system is approximately 490 light years away based on parallax, and it is drifting further away with a mean radial velocity of +6 km/s. As of 2008, the pair had an angular separation of .
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Zeta Eridani (ζ Eridani, abbreviated Zeta Eri, ζ Eri) is a binary star in the constellation of Eridanus. With an apparent visual magnitude of 4.80, it is visible to the naked eye on a clear dark night. Based on parallax measurements taken during the Hipparcos mission, it is approximately 110 light-years from the Sun. Zeta Eridani is the primary or 'A' component of a multiple star system designated WDS J03158-0849 (the secondary or 'B' component is 14 Eridani).
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HD 189733, also catalogued as V452 Vulpeculae, is a binary star system approximately 64.5 light-years away in the constellation of Vulpecula (the Fox). The primary star is suspected to be an orange dwarf star, while the secondary star is a red dwarf star. Given that this system has the same visual magnitude as HD 209458, it promises much for the study of close transiting extrasolar planets. The star can be found with binoculars 0.3 degrees east of the Dumbbell Nebula (M27).
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When sufficient helium has accumulated along a shell on the surface of the white dwarf, a run-away thermonuclear explosion results in a nova outburst. Hence, V445 Puppis may belong to a binary star system and be surrounded by an accretion disk of matter drawn from the companion star. At present, the system is being obscured by an optically thick cloud of dust. A bi-polar outflow of material has been observed moving away from the system at a velocity of .
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18 Draconis is a likely binary star system in the northern circumpolar constellation of Draco. With an apparent visual magnitude of 4.84, it is just bright enough to be faintly visible to the naked eye. The distance to this system, as estimated from an annual parallax shift of , is roughly 720 light years. It is moving closer to the Sun with a heliocentric radial velocity of −1.4 km/s, and is a probable member of the Sirius stream of co-moving stars.
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SZ Crateris is a binary star system in the southern constellation Crater. Both components belong to the main sequence: the primary star has a spectral classification of K5V while the secondary is a red dwarf of spectral class M0V. The radius of the primary is about 66% the radius of the Sun, while the secondary member is only about 42% of the solar radius. In 1994, the two stars were separated by 5.1 arc seconds, which is equivalent to 112.41 astronomical units.
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15 Orionis is a suspected astrometric binary star system in the equatorial constellation of Orion, near the border with Taurus. It is visible to the naked eye as a faint, yellow-white hued star with an apparent visual magnitude of 4.82. The system is approximately 340 light years away from the Sun based on parallax. It is moving further from the Earth with a heliocentric radial velocity of +29 km/s, having come to within some three million years ago.
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Pi Aquilae, Latinized from π Aquilae, is the Bayer designation for a binary star system in the equatorial constellation of Aquila, about 3° to the north of the bright star Altair. The apparent visual magnitude of the system is 5.85, making it faintly visible to the naked eye from dark suburban skies. Based upon an annual parallax shift of 6.34 mas, the distance to this system is roughly . The binary nature of this system was first discovered by William Herschel in 1785.
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At least four distinct techniques have been used to estimate distances from Earth to the Andromeda Galaxy. In 2003, using the infrared surface brightness fluctuations (I-SBF) and adjusting for the new period-luminosity value and a metallicity correction of −0.2 mag dex−1 in (O/H), an estimate of was derived. A 2004 Cepheid variable method estimated the distance to be 2.51 ± 0.13 million light-years (770 ± 40 kpc). In 2005, an eclipsing binary star was discovered in the Andromeda Galaxy.
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Delta Antliae (δ Ant, δ Antliae) is the Bayer designation for a binary star system in the southern constellation of Antlia. The combined apparent visual magnitude of the system is +5.57, allowing it to be viewed from the suburbs with the naked eye. Judging by the parallax shift of this system, it is located at a distance of 450 ± 10 light-years from Earth. The system is reduced in magnitude by 0.03 due to extinction caused by intervening gas and dust.
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HD 106906 is a binary star system in the southern constellation of Crux. It is too faint to be visible to the naked eye, having a combined apparent visual magnitude of 7.80. The distance to this system is approximately 337 light years based on parallax, and it is receding from the Sun with a radial velocity of +10 km/s. It is a member of the Lower Centaurus Crux group of the Scorpius–Centaurus OB association of co-moving stars.
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Iota Gruis, Latinized from ι Gruis, is a binary star system in the southern constellation of Grus. It has an apparent visual magnitude of 3.90, which is bright enough to be seen with the naked eye at night. The distance to this system, as determined using an annual parallax shift of 17.80 mas as seen from the Earth, is about 183 light years. This is a single-lined spectroscopic binary with an orbital period of and an eccentricity of 0.66.
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Psi3 Aquarii, Latinized from ψ3 Aquarii, is the Bayer designation for a visual binary star system in the constellation of Aquarius. It has an apparent visual magnitude of 4.98, which is bright enough to be seen with the naked eye. Parallax measurements give a distance estimate of roughly . The main component of this system is an A-type main sequence star with a stellar classification of A0 V. Its companion is an 11th magnitude star 1.5 arcseconds from the primary.
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Detail of one edge of the bubble blown by EZ CMa. EZ CMa is off frame to the left (east). EZ CMa has an apparent visual magnitude which varies between 6.71 and 6.95 over a period of 3.766 days, along with changes in the spectrum. It has been proposed that it could be a binary star, with a neutron star as companion that would complete an orbit around the Wolf-Rayet with that period, being it the cause of those variations.
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Epsilon Cancri (ε Cancri, abbreviated Epsilon Cnc, ε Cnc) is a white-hued binary star system in the zodiac constellation of Cancer. It is the brightest member of the Beehive Cluster with an apparent visual magnitude of +6.29, which is near the lower limit of visibility with the naked eye. The annual parallax shift of as seen from Earth yields a distance estimate of approximately 616 light-years from the Sun. The binary pair has the designation WDS J08405+1933.
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HD 107148 is an 8th magnitude primary of the binary star system located approximately 161 light years away in the constellation of Virgo. It is a yellow dwarf with a luminosity 1.41 times the Sun. It is twice as enriched with heavy elements than the Sun. In 2012, a comoving white dwarf stellar companion HD 107148 B was detectedWide companions to Hipparcos stars within 67 pc of the Sun at projected separation of 1790 AU, and was confirmed in 2014.
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Kappa Leporis, Latinized from κ Leporis, is a binary star system in the southern constellation of Lepus. The pair have apparent visual magnitudes of 4.43 and 7.00, with the former being bright enough to be seen with the naked eye. As of 2000, they had an angular separation of 2.179 arc seconds along a position angle of 357.3°. Based upon an annual parallax shift of 4.48 mas as measured from Earth, the system is located roughly 730 light years from the Sun.
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Orbit of Procyon B seen from above its plane. Procyon is a binary star system with a bright primary component, Procyon A, having an apparent magnitude of 0.34, and a faint companion, Procyon B, at magnitude 10.7. The pair orbit each other with a period of 40.82 years along an elliptical orbit with an eccentricity of 0.407, more eccentric than Mercury's. The plane of their orbit is inclined at an angle of 31.1° to the line of sight with the Earth.
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Although HD 93250 is known to be a binary star, individual spectra of the two components have never been observed, although they are thought to be very similar. The spectral type of HD 93250 has variously been given as O5, O6/7, O4, and O3. It has sometimes been classified as a main sequence star and sometimes as a giant star. The Galactic O-Star Spectroscopic Survey has used it as the standard star for the newly created O4 subgiant spectral type.
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HD 96167 is a binary star located approximately 280 light years away in the constellation of Crater. Primary HD 96167 A is an 8th magnitude G-type subgiant star It is larger, brighter and more massive than our Sun. The star is metal rich and around 3.8 ± 1 Gyr old. The faint stellar companion was detected in 2014 at the projected separation 506 AU, and existence of additional stellar companions was ruled out at projected distances from 51 to 740 astronomical units.
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The fainter star—Zeta2 Antliae—is 386 ± 5 light-years distant and of magnitude 5.9. Eta Antliae is another double composed of a yellow white star of spectral type F1V and magnitude 5.31, with a companion of magnitude 11.3. Theta Antliae is likewise double, most likely composed of an A-type main sequence star and a yellow giant. S Antliae is an eclipsing binary star system that varies in apparent magnitude from 6.27 to 6.83 over a period of 15.6 hours.
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SN 2004GT was a type Ic supernova that happened in the interacting galaxy NGC 4038 on December 12, 2004. The event occurred in a region of condensed matter in the western spiral arm. The progenitor was not identified from older images of the galaxy, and is either a type WC Wolf-Rayet star with a mass over 40 times that of the Sun, or a star 20 to 40 times as massive as the Sun in a binary star system.
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49 Cassiopeiae is a binary star system in the northern circumpolar constellation of Cassiopeia. It is visible to the naked eye as a faint, yellow-hued point of light with an apparent visual magnitude of 5.22. The system is located about 412 light years away from the Sun, based on parallax. The pair had an angular separation of along a position angle of 244°, as of 2008, with the brighter component being of magnitude 5.32 and its faint companion having magnitude 12.30.
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Parise engaged in a number of astronomical research projects utilizing data from ground-based observatories, the Copernicus satellite (OAO-3), IUE, and the Astro observatory. His research topics, including circumstellar matter in binary star systems and the evolutionary status of stars in globular clusters, resulted in several professional publications. A veteran of two space flights, Parise logged more than 614 hours and 10.6 million miles in space. He served as a payload specialist aboard STS-35 in 1990 and STS-67 in 1995.
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The Hubble Space Telescope has three fine guidance sensors (FGSs). Two are used to point and lock the telescope onto the target, and the third can be used for position measurements - also known as astrometry. Because the FGSs are so accurate, they can be used to measure stellar distances and also to investigate binary star systems. After locking on to a bad guide star, Hubble's tracking system captured this image: the prominent red streaks are actually stars in globular cluster NGC 288.
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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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No red giants have been found to be members of the cluster. One member of the cluster is a Be star. Among the members of the cluster is AI Crucis, a short-period semi-detached massive close binary star, with orbit period 1.41771 days. The orbital period of the binary is continuously increasing and this has been explained on the grounds of mass transfer from the less massive component to the more massive one and strong stellar wind from the hot component.
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Thus it did not show a pre-eruption rise in brightness. This is an interacting binary star system consisting of a white dwarf primary star and a main sequence star with a stellar classification of G8V. The orbit has a period of 0.33381379 days and an inclination of 88.2° to the line of sight to the Earth, resulting in an eclipsing binary. The nova eruption is believed to have been driven by mass transferred from the secondary star to the white dwarf.
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NASA Exoplanet Exploration Program "travel poster" for Kepler-16b The planet orbits in a circumbinary orbit around a (K-type) and (M-type) binary star system. The stars orbit each other about every 41 days. The stars have masses of 0.68 and 0.20 and radii of 0.64 and 0.22 , respectively. They have surface temperatures of 4450 K and 3311 K. Based on the stellar characteristics and orbital dynamics, an estimated age of 2 billion years for the system is possible.
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31 Vulpeculae is a binary star system in the northern constellation of Vulpecula. It is visible to the naked eye as a faint, yellow-hued point of light with an apparent visual magnitude of 4.56. The system is located approximately 228 light years away from the Sun based on parallax, and it is drifting further away with a radial velocity of +2.25 km/s. The variable radial velocity of this system was first suspected by German Astronomer Friedrich Küstner in 1914.
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16 Serpentis is a binary star system in the Serpens Caput portion of the equatorial constellation of Serpens, located 228 light years from the Sun. It is visible to the naked eye as a fain, orange-hued star with an apparent visual magnitude of 5.261. The system is moving further from the Earth with a heliocentric radial velocity of +3 km/s. The variable radial velocity of this star was discovered at Lick Observatory and was announced by J. H. Moore in 1924.
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The presence of this gas creates an excess emission of infrared, along with emission lines in the star's spectrum. Most of it is concentrated around the equator, forming a disk. Some of the variation in this star may be explained by assuming it is a binary star system. This proposed secondary star would need to have about 4–7 times the Sun's mass and be orbiting with a period of at least 4.6 years at a minimum separation of 6.9 Astronomical Units.
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Eta Capricorni, Latinized from η Capricorni, is a binary star system in the southern constellation of Capricornus. It can be seen with the naked eye, having a combined apparent visual magnitude of +4.84. Based upon an annual parallax shift of 20.20 mas as seen from the Earth, the star is located about 161 light years from the Sun. The pair orbit each other with a period of 27.85 years, a semimajor axis of 0.265 arc seconds, an eccentricity of 0.410.
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Most natural satellites of the planets undergo tidal acceleration to some degree (usually small), except for the two classes of tidally decelerated bodies. In most cases, however, the effect is small enough that even after billions of years most satellites will not actually be lost. The effect is probably most pronounced for Mars's second moon Deimos, which may become an Earth-crossing asteroid after it leaks out of Mars's grip. The effect also arises between different components in a binary star.
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Lambda1 is itself a binary star, with two components—a yellow-white star of spectral type F7IV-V and an apparent magnitude of 6.22, and a yellow main sequence star of spectral type G1V and an apparent magnitude of 7.28. The system is 186 light-years distant. Lambda2 is an orange subgiant of spectral type K2III that is expanding and cooling and has left the main sequence. Of apparent magnitude 5.46, it is approximately 220 light-years distant from Earth.
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This binary star system consists of two closely spaced low-mass red dwarfs. The secondary star is a dim magnitude 14 lost in the glare of the nearby primary star. The most recent determination of the system orbital elements comes from a study by George Gatewood using older sources along with data from the Hipparcos satellite. This study yielded an orbital period of about 16.6 years and a semi-major axis separation of about 1.1 arc seconds (2.4–5.3 AU).
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An FS Canis Majoris variable (FS CMa star) is a type of eruptive variable star. The class of variable stars are named after its prototype, FS Canis Majoris. They are somewhat poorly understood, most likely binary star systems in which mass exchange is ongoing or has recently happened, and most likely consist of at least one B-type main-sequence stars in a dust envelope. They undergo irregular light variations over long periods of time, with magnitude variation of approximately 2 magnitudes.
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It is a slow irregular variable star of type Lb, undergoing changes in magnitude over the range 3.57−3.72 with a periodicity of 23.8 d. The measured angular diameter of Tau4 Eridani is . At its estimated distance, this yields a physical size of about 106 times the radius of the Sun. It shines with 1,537 times the luminosity of the Sun from an outer atmosphere at an effective temperature of 3,712 K. This is most likely a binary star system.
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The Hills mechanism is a phenomenon that occurs when a binary star system is disrupted by a supermassive black hole. Tidal forces from the black hole cause one of the stars to be captured by it, and fall into an orbit around it. The other star is jettisoned away from the black hole at very high speeds. The phenomenon was proposed by astronomer Jack Hills in 1988 and confirmed in 2019, when an example of such a jettisoned star was observed.
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Eta Canis Minoris (η CMi, η Canis Minoris) is a binary star system in the equatorial constellation of Canis Minor. It is approximately 318 light-years from Earth. The primary component, η Canis Minoris A, is a yellow-white F-type giant with an apparent magnitude of +5.24. Its companion, η Canis Minoris B, is an eleventh-magnitude star located 4 arcseconds from the primary, though is actually around 440 AU from the main star and takes around 5,000 years to orbit it.
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Tau Sculptoris (τ Scl, τ Sculptoris) is a binary star system in the southern constellation of Sculptor, about 8° to the east-southeast of Alpha Sculptoris. It is faintly visible to the naked eye with a combined apparent visual magnitude of +5.69. Based upon an annual parallax shift of 14.42 mas as seen from Earth, it is located around 230 light years from the Sun. The binary nature of this system was discovered by English astronomer John Herschel in 1835.
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Zeta Virginis (ζ Virginis, abbreviated Zeta Vir, ζ Vir) is a binary star in the zodiac constellation of Virgo. It is visible to the naked eye with an apparent visual magnitude of +3.376 and is located about a half degree south of the celestial equator. Based on parallax measurements obtained during the Hipparcos mission, it is about distant from the Sun. The two components are designated Zeta Virginis A (officially named Heze , a mid-20th-century name for the system) and B.
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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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Zeta Aurigae (ζ Aurigae, abbreviated Zeta Aur, ζ Aur), traditionally known as Sadatoni (among other names), is a binary star in the northern constellation of Auriga. Based upon parallax measurements made during the Hipparcos mission, this system is approximately distant from the sun. It has a combined apparent visual magnitude of 3.75, which is bright enough to be seen with the naked eye. The two components are designated Zeta Aurigae A (officially named Saclateni , an old misspelling of "Sadatoni") and B.
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Pleione (pronounced or ) is a binary star and the seventh-brightest star in the Pleiades star cluster (Messier 45). It has the variable star designation BU Tauri (BU Tau) and the Flamsteed designation 28 Tauri (28 Tau). The star is located approximately from the Sun, appearing in the constellation of Taurus. Pleione is located close on the sky to the brighter star Atlas, so is difficult for stargazers to distinguish with the naked eye despite being a fifth magnitude star.
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Epsilon Trianguli, Latinized from ε Trianguli, is a binary star system in the northern constellation of Triangulum. Based upon measurement of its trigonometric parallax, it is approximately 390 light years from Earth. The primary component is an A-type main sequence star with a stellar classification of A2 V, an apparent magnitude of +5.50 and an estimated age of 600 million years. It has 2.75 times the mass of the Sun and is spinning with a projected rotational velocity of 107 km/s.
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HD 225218 is a quadruple star system in the northern constellation of Andromeda. The primary component, HD 225218 A, is a giant star with a stellar classification of B9III, an apparent magnitude of 6.16, and is a candidate Lambda Boötis star. It has a fainter, magnitude 9.65 companion, HD 225218 B, at an angular separation of 5.2″ along a position angle of 171°. The primary itself has been identified as a binary star system through interferometry, with the two components separated by 0.165″.
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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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The effective temperature of the star's outer envelope is 4,150 K, which gives it the characteristic orange hue of a K-type star. With a diameter 130 times that of the Sun, it would almost reach the orbit of Venus if placed at the centre of the Solar System. There is evidence that Atria may be a binary star. It displays unusual properties for a star of its class, including stellar flares and a higher than normal emission of X-rays.
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Chi Lupi (Chi Lup, χ Lupi, χ Lup) is a spectroscopic binary star in the constellation of Lupus. It has an apparent visual magnitude of approximately 3.957. The primary star in the binary is a mercury-manganese star of spectral type B9.5V; the secondary is a metallic-lined star of type A2Vm. This system is a proper motion member of the Upper Scorpius sub-group in the Scorpius- Centaurus OB association, the nearest such co-moving association of massive stars to the Sun.
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A colliding-wind binary is a binary star system in which the two members are massive stars that emit powerful, radiatively-driven stellar winds. The location where these two winds collide produces a strong shock front that can cause radio, X-ray and possibly synchrotron radiation emission. Wind compression in the bow shock region between the two stellar winds allows dust formation. When this dust streams away from the orbiting pair, it can form a pinwheel nebula of spiraling dust.
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Epsilon Boötis, also known as Izar or Pulcherrima, is a close triple star popular with amateur astronomers and the most prominent binary star in Boötes. The primary is a yellow- or orange- hued magnitude 2.5 giant star, the secondary is a magnitude 4.6 blue-hued main-sequence star, and the tertiary is a magnitude 12.0 star. The system is 210 light-years away. The name "Izar" comes from the Arabic word for "girdle" or "loincloth", referring to its location in the constellation.
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An intermediate-mass X-ray binary (IMXB) is a binary star system where one of the components is a neutron star or a black hole. The other component is an intermediate mass star. Hercules X-1 is composed of a neutron star accreting matter from a normal star (HZ Her) probably due to Roche lobe overflow. X-1 is the prototype for the massive X-ray binaries although it falls on the borderline, , between high- and low-mass X-ray binaries.
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U Vulpeculae is a variable and binary star in the constellation Vulpecula. It is a classical Cepheid variable and its apparent magnitude ranges from 6.73 to 7.54 over a precise cycle of 7.99 days. Its variable nature was discovered in 1898 at Potsdam Observatory by Gustav Müller and Paul Kempf. In 1991 a study of radial velocities showed that it U Vulpeculae is a spectroscopic binary and a full orbit with a period of 2510 days (6.9 years) was first calculated in 1996.
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Omega Fornacis, which is Latinized from ω Fornacis, is a wide binary star system in the southern constellation of Fornax. It has a blue-white hue and is faintly visible to the naked eye as a fifth-magnitude star. The system lies at a distance of approximately 470 light years from the Sun based on parallax, and is drifting further away with a radial velocity of +10 km/s. The dual nature of this system was discovered in 1836 by John Herschel.
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51 Eridani has a companion, known as GJ 3305. The system has a common proper motion with 51 Eridani, and hence it is gravitationally bound, although it is separated by 66″ corresponding to 2,000 AU. It is a binary star system with two M-type red dwarfs. The primary has a mass of while the secondary has a mass of . The two red dwarfs themselves are separated by a semimajor axis of 9.78 ± 0.14 AU and have an eccentricity of 0.19 ± 0.02.
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This is a probable single-lined spectroscopic binary star system. The visible component has a stellar classification of F3 V or F3 IV, indicating it is either an F-type main-sequence star or a somewhat more evolved subgiant star, respectively. It has an estimated 1.3 times the mass of the Sun and about 1.3 times the Sun's radius. The star is 1.75 billion years old and has a high rate of spin with a projected rotational velocity of around 97.5 km/s.
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A close binary star system occurs when two stars orbit each other with an average separation that is of the same order of magnitude as their diameters. At these distances, more complex interactions can occur, such as tidal effects, transfer of mass and even collisions. Tidal interactions in a close binary system can result in modification of the orbital and rotational parameters. The total angular momentum of the system is conserved, but the angular momentum can be transferred between the orbital periods and the rotation rates.
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Originally considered a single star, it was reported to be a shell star in 1982. Circumstellar absorption lines were then found to be variable, showing a similarity to the edge-on debris disk surrounding Beta Pictoris. The stellar classification of A2 IV/V matched an A-type star near the end of its main sequence lifetime, showing traits of an emerging subgiant star phase. A 2019 study using PIONIER (VLTI) and 32 years of radial velocity measurements concluded that HD 256 is instead a binary star.
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59 Persei is a suspected astrometric binary star system in the northern constellation of Perseus. It is visible to the naked eye as a dim, white-hued star with an apparent magnitude of 5.30. The star is located around 256 light years distant from the Sun, based on parallax, and is drifting further away with a radial velocity of +13 km/s. This is an ordinary A-type main-sequence star with a stellar classification of A1Vn, a star that is fusing its core hydrogen.
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60 Sagittarii is a suspected binary star system in the southern constellation of Sagittarius. It has the Bayer designation A Sagittarii, while 60 Sagittarii is the Flamsteed designation. This naked eye object forms the northwest corner of the asterism called the Terebellum and, with an apparent magnitude of approximately 4.84, it is the dimmest of the four stars in the Terebellum. It is located 379 light years from the Sun, based on parallax, but is moving closer with a radial velocity of −51 km/s.
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HD 156846 is a binary star system in the equatorial constellation of Ophiuchus, positioned a degree SSE of Messier 9. It has a yellow hue and is just barely bright enough to be visible to the naked eye with an apparent visual magnitude of 6.5. The system is located at a distance of 156 light years from the Sun based on parallax. It is drifting closer with a radial velocity of −68.5 km/s, and is predicted to come to within in about 476,000 years.
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