Double star system Eta Carinae seems perpetually ready to explode, as we've reported before.
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Those halcyon days may be over, but now, we have a double star system to enjoy instead.
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The latest known red nova was V1309 Scorpii, a double-star system that unexpectedly merged and detonated in 2008.
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What's notable about this particular discovery is that it's the largest planet in a double-star system discovered so far.
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The astronomers hypothesize that the runaway star was once part of a double-star system that came too close to the black hole.
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Scientists think either binary black holes were formed from a double star system or they are "completely solitary" black holes that end up in a star cluster orbiting one another, LIGO researcher Nergis Mavalvala said.
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Amateur telescopes can discern them but require magnification of about 100 times. They are situated 50′ east of the well-known double star system Gamma Leonis (i.e. Algieba).
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Gamma Boötis forms the primary or 'A' component of a double star system designated WDS J14321+3818 ('B' is the star UCAC2 45176266). Gamma Boötis' two components are themselves designated WDS J14321+3818Aa (officially named Seginus , the traditional name of the Gamma Bootis system) and Ab.
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HD 208177 is a double star system in the equatorial constellation of Aquarius. They are faintly visible to the naked eye with an apparent magnitude of 6.20. The pair have an angular separation of 19.113″. The primary component is an evolved subgiant star with a stellar classification of F5IV.
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NGC 18 is a double star system (both G4) system located in the constellation of Pegasus. It was first recorded by Herman Schultz on 15 October 1866. It was looked for but not found by Édouard Stephan on 2 October 1882. It was independently observed by Guillaume Bigourdan in November 1886.
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1 Camelopardalis (1 Cam) is a double star system in the constellation Camelopardalis. Its combined apparent magnitude is 5.56 and it is approximately away. The 1 Camelopardalis system is part of the Camelopardalis OB1 stellar association, which is 820 pc away. 1 Camelopardalis A is a hot massive star which has evolved away from the main sequence to become a giant.
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HD 99922 is a double star system in the constellation of Crater. It shines with an apparent visual magnitude of 5.77 from a distance of about 450 light years (140 parsecs) away from the Earth. The primary star is an A-type main sequence star; the secondary star is located about 8 arcseconds away. Other designations include HR 4428 and HIP 56078.
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HD 88809 is a star in a double star system in the constellation Antlia. The primary is an orange giant of spectral type K1III. Located around 480 light- years distant, it shines with a luminosity approximately 124 times that of the Sun and has a surface temperature of 4607 K. It has an apparent magnitude of 5.9, while the secondary star has a magnitude of 13.
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Mu Geminorum (μ Geminorum, abbreviated Mu Gem, μ Gem), formally named Tejat , is a single star in the northern constellation of Gemini. From parallax measurements obtained during the Hipparcos mission, it is roughly distant from the Sun. Mu Geminorum forms the primary or 'A' component of a double star system designated WDS J06230+2231 along with UCAC2 39641417 (also designated WDS J06230+2231BC), itself a binary pair.
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Alpha Caeli (α Cae, α Caeli) is a double star system in the constellation Caelum. Alpha Caeli A is an F-type main sequence star with a stellar classification of F2V and an apparent magnitude of +4.44. It has 1.48 times the mass of the Sun and 1.3 times the solar radius. The projected rotational velocity at the stellar equator is 47.8 km/s.
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2 Equulei is a double star system in the constellation of Equuleus. The primary component of the 2 Equ pair is an F-type main sequence star. As of 2015, the secondary had an angular separation of 2.90 arc seconds along a position angle of 213° from the primary. They form a common proper motion pair, two stars at approximately the same distance and moving in the same direction.
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Supernovae can result from the death of an extremely massive star, many times heavier than the Sun. At the end of the life of this massive star, a non-fusible iron core is formed from fusion ashes. This iron core is pushed towards the Chandrasekhar limit till it surpasses it and therefore collapses. A supernova may also result from mass transfer onto a white dwarf from a star companion in a double star system.
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Map of Paz, the continent group in which the Dray Prescot series is set. The series is set on the fictional world of Kregen, a planet of the Antares star system in the constellation of Scorpio. Antares is envisioned as a double star system consisting of a large red giant (Antares A) and a smaller green star (Antares B). Antares B is in reality blue, though often described as green, probably owing to a contrast effect.James Kaler, "Antares".
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16 Cygni Bb or HD 186427 b is an extrasolar planet approximately 69 light- years away in the constellation of Cygnus. The planet was discovered orbiting the Sun-like star 16 Cygni B, one of two solar-mass () components of the triple star system 16 Cygni in 1996. It orbits its star once every 799 days and was the first eccentric Jupiter and planet in a double star system to be discovered. The planet is abundant in Lithium.
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ESO Supernova building. The visitor centre was designed by the architects Bernhardt + Partner, that already designed the Haus der Astronomie, a centre for astronomy education and outreach. The design of the ESO Supernova resembles that of a close double-star system with one star transferring mass to its companion. This set-up will ultimately lead to the heavier component exploding as a supernova, briefly becoming as bright as the light of all the stars in the Milky Way combined.
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Lambda1 Sculptoris, Latinized from λ1 Sculptoris, is a double star system in the southern constellation of Sculptor. It is close to the lower limit of visibility to the naked eye, with a combined apparent visual magnitude of +6.05. Based upon an annual parallax shift of 6.89 mas as measured from Earth, it is located roughly 470 light years from the Sun. At that distance, the visual magnitude is diminished by an extinction factor of 0.026 due to interstellar dust.
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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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Assuming that one of the fifteen stars on the map must represent Earth's Sun, Fish constructed a three-dimensional model of nearby Sun-like stars (i.e. stars deemed to have characteristics that could support life such as that found on Earth) using thread and beads, basing stellar distances on those published in the 1969 Gliese Star Catalogue. Studying thousands of vantage points over several years, the only one that seemed to match the Hill map was from the viewpoint of the double star system of Zeta Reticuli. Fish sent her analysis to Webb.
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NOEMA has observed the most distant galaxy known to date. Together with the IRAM 30-meter telescope it made the first complete and detailed radio images of nearby galaxies and their gas. NOEMA also obtained the first image of a gas disk surrounding a double star system (Guilloteau et al. 1994). Its antennas captured for the first time a cavity in one of these disks, a major hint for the existence of a planetary object orbiting the new star and absorbing matter on its trajectory (GG tau, Piétu et al. 2011).
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The white stars Beta and Gamma Trianguli, of apparent magnitudes 3.00 and 4.00, respectively, form the base of the triangle and the yellow-white Alpha Trianguli, of magnitude 3.41, the apex. Iota Trianguli is a notable double star system, and there are three star systems with known planets located in Triangulum. The constellation contains several galaxies, the brightest and nearest of which is the Triangulum Galaxy or Messier 33—a member of the Local Group. The first quasar ever observed, 3C 48, also lies within the boundaries of Triangulum.
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HD 74389 is a double star system approximately 425 light years from Earth. The primary, HD 74389 A, was initially listed in the Hipparcos catalog as an A0V spectral type star, but this was subsequently updated in 1990 as A2V when Sanduleak and Pesch imaged it with the Burrell Schmidt telescope at Kitt Peak. The primary component is a white A-type main sequence star with an apparent magnitude of +7.48. Its furthest companion, HD 74389 B, is a DA-type white dwarf located 20.11 arcseconds west of—at least 190 AU from—HD 74389 A, and has a V magnitude of 14.62.
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The story is set on Tormance, an imaginary planet orbiting the star Arcturus, which, in the novel (but not in reality) is a double star system, consisting of Branchspell, a large yellow sunlike star, and Alppain, a smaller blue star. It is said in the novel to be 100 light- years distant from Earth. There is no systematic description of the geography of Tormance; Maskull simply travels from South to North (with a somewhat eastward excursion to the Sant levels). The direction is symbolic: the light of the second sun, Alppain, is seen to the north; the southern countries are illuminated only by Branchspell.
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An ESO artist's impression of the now-disproven planet Alpha Centauri Bb, orbiting at a distance well short of the star's habitable zone. As one of the brightest stars in Earth's night sky, and the closest-known star system to the Sun, the Alpha Centauri system plays an important role in many fictional works of literature, popular culture, television, and film. Alpha Centauri, a double star system with the binary designation Alpha Centauri AB, is the brightest visible object in the southern constellation Centaurus. Its component stars are Alpha Centauri A (the primary—somewhat larger and brighter than the Sun) and Alpha Centauri B (the secondary—slightly smaller and dimmer).
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Orbital motion has been detected in the central system, but not in the outer pair (as its separation is too high); a preliminary orbit for GG Tauri A has been calculated. Interferometric techniques have been used to observe GG Tauri Ab, the lower- mass component of the central system. GG Tauri Ab may actually be a double star system comprising two red dwarfs (Ab1 = M2V, Ab2 = M3V), with a separation of about 4.5 AU. Its orbital period is currently estimated to be around 16 years. This would explain why the GG Tauri Ab's spectrum suggests an unusually low-mass star instead of the higher mass that was measured.
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According to simple emission theory, light thrown off by an object should move at a speed of c with respect to the emitting object. If there are no complicating dragging effects, the light would then be expected to move at this same speed until it eventually reached an observer. For an object moving directly towards (or away from) the observer at v metres per second, this light would then be expected to still be travelling at (c+v) ( or (c-v) ) metres per second at the time it reached us. In 1913, Willem de Sitter argued that if this was true, a star orbiting in a double-star system would usually, with regard to us, alternate between moving towards us and away from us.
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Based on parallax measurements from the Hipparcos astrometry satellite, this star is located about from the Earth. It has an apparent visual magnitude of 2.84 and a stellar classification of G5 II. The mass of this star is 3.5 times the mass of the Sun and it is about 240 million years old, which is sufficient time for a star this massive to consume the hydrogen at its core and evolve away from the main sequence, becoming a G-type bright giant. This is a double star system and may be a binary. Using adaptive optics on the AEOS telescope at Haleakala Observatory, the pair was found to be separated by an angle of 2.58 arcseconds at a position angle of 1.4°.
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Moreover, he is recognized as the first Spanish in calculating the orbit of a double star system in the country, the STT 77. It follows the appointment of Aller as a member of the “International Astronomical Union Commission 26 (double stars)” in 1948 (Zurich). The following year he was named a member of the National Commission on Astronomy. The professor Aller Ulloa also designed and built devices for measuring and observation purchased by the Paris Observatory; he suggested modifications on the production of the astrograph to the German manufacture Zeiss, which accepted them and afterwards did not accept the payment of Aller Ulloa for the device as appreciation for the improvements; a clock of sidereal time; a base for the portable vertical circle monocular, etc..."Ramón María Aller Ulloa" Contistuted by his two main research lines double stars and the methods to determine coordinates based on two vertical lanes he published 78 articles in especialized publications in Europe, 4 books and he directed 5 PhD thesis (Between 1960 and 1963, in spite of being 83 years old, Aller still directed three theses: Múgica Buhigas's “ber die Anwendung des Theodolits in der Geodtischen Astronomia” (Munich, 1960); Zaera de Toledo's “On determining the Orbits of Visual Double Stars.
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