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List Of Exoplanets Discovered In 2013 ...
This is a List of exoplanets discovered in 2013. For exoplanets detected only by radial velocity, the mass value is actually a lower limit. (See Minimum mass for more information) Specific exoplanet lists References {{DEFAULTSORT:Exoplanets discovered in 2013, List of 2013 * exoplanets An exoplanet or extrasolar planet is a planet outside the Solar System. The first possible evidence of an exoplanet was noted in 1917 but was not recognized as such. The first confirmation of detection occurred in 1992. A different planet, init ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Minimum Mass
In astronomy, minimum mass is the lower-bound calculated mass of observed objects such as planets, stars and binary systems, nebulae, and black holes. Minimum mass is a widely cited statistic for extrasolar planets detected by the radial velocity method or Doppler spectroscopy, and is determined using the binary mass function. This method reveals planets by measuring changes in the movement of stars in the line-of-sight, so the real orbital inclinations and true masses of the planets are generally unknown. This is a result of sin ''i'' degeneracy. If inclination ''i'' can be determined, the true mass can be obtained from the calculated minimum mass using the following relationship: M_\text = \frac Exoplanets Orientation of the transit to Earth Most stars will not have their planets lined up and orientated so that they eclipse over the center of the star and give the viewer on earth a perfect transit. It is for this reason that when we often are only able to extrapolat ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Gliese 504 B
Gliese 504 b (often shortened to GJ 504 b) is considered by NASA to be a Jovian planet and it is located in the system of the solar analog 59 Virginis (GJ 504),In spite of names of some exoplanets, derived from theirs host stars Flamsteed designations (for example, 51 Pegasi b, 61 Virginis b, 70 Virginis b etc.), the discoverers of this exoplanet did not use a similar name (i.e. "59 Virginis b") to refer to it, but used the designation "GJ 504 b" instead, derived from the Gliese–Jahreiß identifier of its parent star "GJ 504". discovered by direct imaging using HiCIAO instrument and AO188 adaptive optics system on the 8.2-meter Subaru Telescope of Mauna Kea Observatory, Hawaii by Kuzuhara et al. Visually, GJ 504 b would have a magenta color. It can be seen from Earth in the constellation Virgo. History of observation The discovery images were taken in 2011 and common proper motion was confirmed in 2012 as part of the Strategic Explorations of Exoplanets and Disks with Subar ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
HD 113337
HD 113337 (LDS 2662 A) is the primary component of binary star system LDS 2662, about away from Earth. The primary main-sequence star belongs to the spectral class of F6. The star system is extremely young, and it is slightly enriched in heavy elements, with an abundance of such elements at about 115% that of the Sun. The primary star is surrounded by a debris disk discovered by the Herschel Space Observatory, and the plane of the disk is likely misaligned with the planetary orbits by 17–32°. The effective temperature of this disk is 55 K. The possibility of other stellar companions near the primary star was ruled out in 2016, for projected separations above 5″ (181 AU). The existence of a secondary companion (called LDS 2662 B, or LSPM J1301+6337) was discovered in 2001 and confirmed to be bound to the primary in 2007. Initially believed to be a single red dwarf star, in 2012 the companion was discovered to actually be a pair of nearly identical red dwarfs, ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
HD 109271
HD 109271 is a wide binary star system in the constellation of Virgo. The brighter member of the binary has a pair of orbiting exoplanets. With an apparent visual magnitude of 8.05, it cannot be seen with the naked eye. Parallax measurements made by Gaia put the star at a distance of away from the Sun, but it is drifting closer with a radial velocity of −5 km/s. The system shows a high proper motion, traversing the celestial sphere at an angular rate of . The primary component is an ordinary G-type main-sequence star with a stellar classification of G5 V. It is a much older star than the Sun with an age of about 7.3 billion years, and is spinning with a projected rotational velocity of 2.7 km/s. This star has 7% more mass than the Sun and a 30% greater girth. The abundance of iron, a measure of the star's metallicity, is similar but slightly higher than in the Sun. It is radiating 1.65 times the luminosity of the Sun from its photosphere at an effective ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
The Astrophysical Journal Letters
''The Astrophysical Journal'', often abbreviated ''ApJ'' (pronounced "ap jay") in references and speech, is a peer-reviewed scientific journal of astrophysics and astronomy, established in 1895 by American astronomers George Ellery Hale and James Edward Keeler. The journal discontinued its print edition and became an electronic-only journal in 2015. Since 1953 ''The Astrophysical Journal Supplement Series'' (''ApJS'') has been published in conjunction with ''The Astrophysical Journal'', with generally longer articles to supplement the material in the journal. It publishes six volumes per year, with two 280-page issues per volume. ''The Astrophysical Journal Letters'' (''ApJL''), established in 1967 by Subrahmanyan Chandrasekhar as Part 2 of ''The Astrophysical Journal'', is now a separate journal focusing on the rapid publication of high-impact astronomical research. The three journals were published by the University of Chicago Press for the American Astronomical Society unt ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
HD 106906 B
HD 106906 b is a directly imaged planetary-mass companion and candidate exoplanet orbiting the star , in the constellation Crux at about from Earth. It is estimated to be about eleven times the mass of Jupiter and is located about 738 AU away from its host star. is rare in astronomy; while its mass estimate is nominally consistent with identifying it as an exoplanet, it appears at a much wider separation from its parent star than thought possible for in-situ formation from a protoplanetary disk. Description is the only known companion orbiting , a spectroscopic binary star composed of two F5V main-sequence stars with a combined mass of . Based on the star's luminosity and temperature, the system is estimated to be about . The system is a likely member of the Scorpius–Centaurus association. The star is surrounded by a debris disk oriented 21 degrees away from ; this disk is about from the binary on its interior and ranges asymmetrically from approximately from the ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
HD 103774
HD 103774 is a star with a close orbiting planetary companion in the southern constellation of Corvus. With an apparent visual magnitude of 7.13, it is too faint to be readily visible to the naked eye. Parallax measurements provide a distance estimate of 184 light years from the Sun. It is drifting closer with a radial velocity of −3 km/s. The star has an absolute magnitude of 3.41. The stellar classification of HD 103774 is F6 V, indicating this is an F-type main-sequence star that is generating energy through core hydrogen fusion. It is a young star with age estimates ranging from 260 million up to 2 billion years of age. The star is mildly active and is spinning with a projected rotational velocity of 8 km/s. It has 1.4 times the mass and 1.56 times the radius of the Sun. The star is radiating 3.7 times the luminosity of the Sun from its photosphere at an effective temperature of 6,391 K. Planetary system This star has been und ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
HD 95086 B
HD 95086 b is a confirmed, directly imaged exoplanet orbiting the young, 17 Myr A-class pre-main-sequence star HD 95086. It is roughly 5 times as massive as Jupiter and orbits about 70 AU away from the parent star. It was detected at thermal infrared wavelengths (3.8 μm) through direct imaging, using the NACO instrument on the VLT. A debris disk has been detected in this system at submillimeter wavelengths and has been resolved in the far-infrared from data obtained with the Herschel Space Observatory. The planet was initially detected in data taken in 2012 at a separation from the parent star of (~56 AU) and position angle of . The planet was recovered at a high signal-to-noise ratio in June 2013. Astrometry for the planet in January 2012 and June 2013, and from a marginal detection in March 2013 confirm that it is bound to the parent star, not a background star. HD 95086 b's brightness at 3.8 μm when combined with sensitive upper limits on its brightne ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
HD 65216
HD 65216 is a triple star system with two exoplanetary companions in the southern constellation of Carina. With an apparent visual magnitude of 7.97 it cannot be readily seen without technical aid, but with binoculars or telescope it should be visible. The system is located at a distance of 114.7 light-years from the Sun based on parallax measurements, and is drifting further away with a radial velocity of 42.6 km/s. The primary, component A, is an ordinary G-type main-sequence star with a stellar classification of G5V. It is nearly two billion years old and is spinning with a projected rotational velocity of 1.3 km/s. The star has 95% of the mass and 86% of the radius of the Sun. It is radiating 72% of the luminosity of the Sun from its photosphere at an effective temperature of 5,718 K. In 2008 a co-moving binary system of low mass companions were discovered at an angular separation of from the primary, which is equivalent to a projected separatio ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
HATS-3
HATS-3 is an F-type main-sequence star away. Its surface temperature is 6351 K. HATS-3 is relatively depleted in its concentration of heavy elements, with a metallicity Fe/H index of −0.157, but is slightly younger than the Sun at an age of 3.2 billion years. A multiplicity survey in 2016 detected a candidate stellar companion to HATS-3, 3.671 arc-seconds away. Planetary system In 2013, one planet, named HATS-3b, was discovered on a tight, nearly circular orbit. The planetary orbit of HATS-3b is likely aligned with the equatorial plane of the star, at a misalignment angle of 3°. The planetary equilibrium temperature is 1643 K. References Capricornus Planetary transit variables F-type main-sequence stars Planetary systems with one confirmed planet J20494978-2425436 103 103 may refer to: *103 (number), the number *AD 103, a year in the 2nd century AD *103 BC, a year in the 2nd century BC * 103 (Tyne Electrical Engineers) Field Squadron, a territorial ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
