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HD 114762 is a triple star system[4][5] approximately 126 light-years (38.6 pc) away in the constellation Coma Berenices. It consists of a yellow-white F-type main-sequence star (HD 114762 A) and two red or brown dwarf companions (HD 114762 Ab & HD 114762 B) approximately 0.36 & 130 AU distant.[4][5] Both are low-metal subdwarfs. Planets around such metal-poor stars are rare (three known cases are HD 22781, HD 111232, and HD 181720).[6] A telescope or strong binoculars are needed to view the primary. HD 114762 had been used by scientists as a "standard star", one whose radial velocity is well established, but with the discovery of the spectroscopic companion HD 114762 Ab its usefulness as a standard has been called into question.[7]

HD 114762
Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Coma Berenices
Right ascension 13h 12m 19.7428s[1]
Declination +17° 31′ 01.654″[1]
Apparent magnitude (V) 7.30[citation needed]
Characteristics
A
Evolutionary stage Main sequence
Spectral type F9V[citation needed]
U−B color index -0.05[citation needed]
B−V color index 0.54[citation needed]
V−R color index 0.29[citation needed]
R−I color index 0.20[citation needed]
J−H color index 0.25[citation needed]
J−K color index 0.33[citation needed]
B
Evolutionary stage Main sequence
Spectral type M6?V
J−K color index 0.70
Astrometry
Radial velocity (Rv)51.03±0.14[citation needed] km/s
Proper motion (μ) RA: −582.611±0.041[1] mas/yr
Dec.: −0.520±0.039[1] mas/yr
Parallax (π)25.88 ± 0.46 mas[1]
Distance126 ± 2 ly
(38.6 ± 0.7 pc)
Details[2]
Mass0.84 M☉
Radius1.24±0.1 R☉
Temperature5934.0±80.0 K
Metallicity [Fe/H]−0.71±0.08 dex
Age11.8±3.9 Gyr
Other designations
BD+18 2700, HD 114762, HIP 64426, SAO 100458, 2MASS J13121982+1731016[3]
Database references
SIMBADdata
Exoplanet Archivedata
ARICNSdata
Extrasolar Planets
Encyclopaedia		data

Spectroscopic companion


In 1989, a companion object, HD 114762 Ab, was found orbiting HD 114762 A by Latham, et al., using Doppler spectroscopy,[8] but its existence was not confirmed until 1991 by Cochran, et al.[9] It has a minimum mass of 10.69 MJ, and thus was originally thought to be a massive exoplanet; however, in 2019, its inclination was determined by Gaia astrometry, giving it a true mass of 107 MJ. This makes it a red dwarf star, or a massive brown dwarf.[5] A 2020 study provided further confirmation of this, and revised the mass upwards to 147 MJ.[10] Its orbital distance and revolution is similar to that of Mercury, though it has twice the eccentricity.[9]

The HD 114762 planetary system[5][10]
Companion
(in order from star)		 Mass Semimajor axis
(AU)		 Orbital period
(days)		 Eccentricity Inclination Radius
b 147.0+39.3
−42.0 MJ		 0.363±0.0121 83.9151±0.0030 0.566+0.012
−0.011		 4.940+1.773
−0.942°		 —

References


  1. Brown, A. G. A.; et al. (2016). "Gaia Data Release 1. Summary of the astrometric, photometric, and survey properties". Astronomy and Astrophysics. 595. A2. arXiv:1609.04172. Bibcode:2016A&A...595A...2G. doi:10.1051/0004-6361/201629512. S2CID 1828208. Gaia Data Release 1 catalog entry.
  2. "The Extrasolar Planet Encyclopaedia — HD 114762 B". Archived from the original on 2013-05-16. Retrieved 2014-09-08.
  3. "HD 114762". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2019-01-16.
  4. Patience, J.; White, R. J.; Ghez, A. M.; McCabe, C.; McLean, I. S.; et al. (December 2002). "Stellar Companions to Stars with Planets". The Astrophysical Journal. 581 (1): 654–665. arXiv:astro-ph/0207538. Bibcode:2002ApJ...581..654P. doi:10.1086/342982. S2CID 119519887.
  5. Kiefer, Flavien (17 October 2019). "Determining the mass of the planetary candidate HD 114762 b using Gaia". Astronomy & Astrophysics. 632: L9. arXiv:1910.07835. Bibcode:2019A&A...632L...9K. doi:10.1051/0004-6361/201936942. S2CID 204743831.
  6. Adibekyan, Vardan (2019), "Heavy Metal Rules. I. Exoplanet Incidence and Metallicity", Geosciences, 9 (3): 105, arXiv:1902.04493, Bibcode:2019Geosc...9..105A, doi:10.3390/geosciences9030105, S2CID 119089419
  7. Maugh II, Thomas H. (4 August 1988). "Other Planets, Other Suns: Astronomers Say Star's Wobble Tells a Story". Los Angeles Times. Retrieved 7 September 2014.
  8. Latham, David W.; Mazeh, Tsevi; Stefanik, Robert P.; Mayor, Michel; Burki, Gilbert (May 1989). "The unseen companion of HD114762 - A probable brown dwarf". Nature. 339 (6219): 38–40. Bibcode:1989Natur.339...38L. doi:10.1038/339038a0. S2CID 4324036.
  9. Cochran, William D.; Hatzes, Artie P.; Hancock, Terry J. (10 October 1991). "Constraints on the Companion Object to HD 114762". The Astrophysical Journal. 380: L35–L38. Bibcode:1991ApJ...380L..35C. doi:10.1086/186167.
  10. Kiefer, Flavien; Hébrard, Guillaume; Lecavelier, Alain; Martioli, Eder; Dalal, Shweta; Vidal-Madjar, Alfred (2021). "Determining the true mass of radial-velocity exoplanets with Gaia 9 planet candidates in the brown-dwarf/stellar regime and 27 confirmed planets". Astronomy & Astrophysics. A7: 645. arXiv:2009.14164. doi:10.1051/0004-6361/202039168. S2CID 221995447.


На других языках

[de] HD 114762

HD 114762 ist die Bezeichnung für ein Sternsystem im Sternbild Haar der Berenike. Es ist etwa 130 Lichtjahre von der Erde entfernt. Der Zentralstern ist ein metallarmer Hauptreihenstern der Spektralklasse F9, der von zwei Begleitern umrundet wird.[3]
- [en] HD 114762

[ru] HD 114762

HD 114762 — тройная звезда в созвездии Волос Вероники на расстоянии приблизительно 132 световых лет (около 40,2 парсека) от Солнца. Возраст звезды определён как около 12 млрд лет[4].


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