HD 114762
 | It has been suggested that HD 114762 b be merged into this article. (Discuss) Proposed since December 2020. |
| 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] |
| Distance | 126 ± 2 ly (38.6 ± 0.7 pc) |
| Details[2] | |
| Mass | 0.84 M☉ |
| Radius | 1.24±0.1 R☉ |
| Temperature | 5934.0±80.0 K |
| Metallicity [Fe/H] | −0.71±0.08 dex |
| Age | 11.8±3.9 Gyr |
| Other designations | |
| Database references | |
| SIMBAD | data |
| Exoplanet Archive | data |
| ARICNS | data |
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]
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 updwards to 147 MJ.[10] Its orbital distance and revolution is similar to that of Mercury, though it has twice the eccentricity.[9]
| 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
- ^ a b c d e 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.
- ^ [1][dead link]
- ^ "HD 114762". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2019-01-16.
- ^ a b 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.
- ^ a b c d 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.
- ^ 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
{{citation}}: CS1 maint: unflagged free DOI (link) - ^ 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.
- ^ 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.
- ^ a b 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.
- ^ a b 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.
