Astronomy:HD 114762 b

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Short description: Star in the constellation Coma Berenices
HD 114762 b[1]
Observation data
Equinox J2000.0]] (ICRS)
Constellation Coma Berenices
Right ascension  13h 12m 19.7428s[2]
Declination +17° 31′ 01.654″[2]
Astrometry
Distance126±2[2] ly
(38.6±0.7[2] pc)
Orbit
PrimaryHD 114762
Period (P)83.915±0.003 d[3]
Semi-major axis (a)0.375±0.006 AU[3]
Eccentricity (e)0.566+0.012
−0.011[3]
Inclination (i)6.23+1.97
−1.26[3]°
Periastron epoch (T)2449889.106±0.186[4]
Argument of periastron (ω)
(secondary)		201.3±1.0[3]°
Semi-amplitude (K2)
(secondary)		612.48±3.52[4] km/s
Details
Mass107+20
−27[3] 147.0+39.3
−42.0[5] MJup
Database references
SIMBADdata

HD 114762 b is a small red dwarf star, in the HD 114762 system,[3] formerly thought to be a massive gaseous[6][7] extrasolar planet,[8] approximately 126 light-years (38.6 pc) away in the constellation of Coma Berenices.[1][6] This optically undetected companion to the late F-type main-sequence star HD 114762 was discovered in 1989 by Latham, et al.,[7] and confirmed in an October 1991 paper by Cochran, et al.[9] It was thought to be the first discovered exoplanet (although its existence was confirmed after those around PSR B1257+12.)

The object orbits the primary star every 83.9 days at an approximate distance of 0.37 AU,[3] with an orbital eccentricity of 0.57;[3] for comparison, this orbit is similar to that of Mercury but with almost three times the eccentricity.[3] Based on the radial velocity measurements alone, it was estimated to have a minimum mass of 11.069±0.063  |♃|J}}}}}} (at 90°)[10] and a probable mass of approximately 63.2 |♃|J}}}}}} (at 10°).[11] However, analysis of its astrometric perturbation of its host star in 2019 found it to have an extremely low inclination of only 6.23+1.97
−1.26 degrees, giving it a true mass of 107+20
−27 MJ and putting it well outside of the range of planetary masses (less than 13 |♃|J}}}}}}).[3]

HD 114762 b was thought for a time to be the first extrasolar planet ever detected, predating the 1992 pulsar planets found around PSR B1257+12 and main-sequence yellow dwarf 51 Pegasi.[12][13] However, now that it has been found to not be a planet, the planets found orbiting PSR B1257+12 were indeed the first exoplanets ever found.[3]

At an event celebrating the career of discoverer David Latham and attended by his colleagues and collaborators, the object was informally dubbed "Latham's Planet".[14] However, this name has no official standing with the International Astronomical Union.

See also

References

  1. ↑ 1.0 1.1 Butler, R. P. et al. (2006). "Catalog of Nearby Exoplanets". The Astrophysical Journal 646 (1): 505–522. doi:10.1086/504701. Bibcode: 2006ApJ...646..505B. 
  2. ↑ 2.0 2.1 2.2 2.3 Brown, A. G. A et al. (2016). "Gaia Data Release 1. Summary of the astrometric, photometric, and survey properties". Astronomy and Astrophysics 595: A2. doi:10.1051/0004-6361/201629512. Bibcode: 2016A&A...595A...2G. https://www.aanda.org/articles/aa/full_html/2016/11/aa29512-16/aa29512-16.html. Gaia Data Release 1 catalog entry
  3. ↑ 3.00 3.01 3.02 3.03 3.04 3.05 3.06 3.07 3.08 3.09 3.10 3.11 Kiefer, Flavien (17 October 2019). "Determining the mass of the planetary candidate HD 114762 b using Gaia". Astronomy & Astrophysics 632: L9. doi:10.1051/0004-6361/201936942. Bibcode: 2019A&A...632L...9K. 
  4. ↑ 4.0 4.1 Kane, Stephen R. et al. (2011). "Revised Orbit and Transit Exclusion for HD 114762b". The Astrophysical Journal Letters 735 (2): L41. doi:10.1088/2041-8205/735/2/L41. Bibcode: 2011ApJ...735L..41K. 
  5. ↑ Kiefer, F. et al. (January 2021). "Determining the true mass of radial-velocity exoplanets with Gaia. Nine planet candidates in the brown dwarf or stellar regime and 27 confirmed planets". Astronomy & Astrophysics 645. doi:10.1051/0004-6361/202039168. Bibcode: 2021A&A...645A...7K. 
  6. ↑ 6.0 6.1 North, Gerald (2003). Astronomy in Depth. New York: Springer. p. 185. ISBN 9781852335809. https://books.google.com/books?id=D3RRG9W8nSYC&pg=PA185. 
  7. ↑ 7.0 7.1 Latham, David W. et al. (4 May 1989). "The unseen companion of HD114762: a probable brown dwarf". Nature 339 (6219): 38–40. doi:10.1038/339038a0. Bibcode: 1989Natur.339...38L. 
  8. ↑ "HD 114762b". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=HD+114762b. 
  9. ↑ Cochran, William D. et al. (10 October 1991). "Constraints on the Companion Object to HD 114762". The Astrophysical Journal 380: L35–L38. doi:10.1086/186167. Bibcode: 1991ApJ...380L..35C. 
  10. ↑ Wang, Sharon Xuesong et al. (2012). "The Discovery of HD 37605c and a Dispositive Null Detection of Transits of HD 37605b". The Astrophysical Journal 761 (1): 46–59. doi:10.1088/0004-637X/761/1/46. Bibcode: 2012ApJ...761...46W. 
  11. ↑ Kane, Stephen R.; Gelino, Dawn M. (2012). "Distinguishing between stellar and planetary companions with phase monitoring". Monthly Notices of the Royal Astronomical Society 424 (1): 779–788. doi:10.1111/j.1365-2966.2012.21265.x. Bibcode: 2012MNRAS.424..779K. https://academic.oup.com/mnras/article/424/1/779/1012726. 
  12. ↑ Hale, Alan (1995). "On the Nature of the Companion to HD 114762". Publications of the Astronomical Society of the Pacific (The University of Chicago Press) 107 (707): 22–26. doi:10.1086/133511. Bibcode: 1995PASP..107...22H. 
  13. ↑ Marcy, Geoffrey W. et al. (1999). "Two New Candidate Planets in Eccentric Orbits". The Astrophysical Journal 520 (1): 239–247. doi:10.1086/307451. Bibcode: 1999ApJ...520..239M. 
  14. ↑ Johnson, John (2016). How do you find an Exoplanet?. New Jersey: Princeton University Press. p. 137. ISBN 978-0-691-15681-1. https://books.google.com/books?id=-DNJCgAAQBAJ&pg=PA137. 

Coordinates: Sky map 13h 12m 19.7427s, +17° 31′ 01.643″



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