HD 126614 is a trinary star[14] system in the equatorial constellation of Virgo. The primary member, designated component A, is host to an exoplanetary companion. With an apparent visual magnitude of 8.81,[7] it is too faint to be seen with the naked eye. The system is located at a distance of 239 light years from the Sun based on parallax measurements,[1] but is drifting closer with a radial velocity of −33 km/s.[8]
| Observation data Epoch J2000.0 Equinox J2000.0 | |
|---|---|
| Constellation | Virgo |
| HD 126614 A | |
| Right ascension | 14h 26m 48.279494s[1] |
| Declination | −05° 10′ 40.01306″[1] |
| Apparent magnitude (V) | 8.81±0.03[2] |
| LP 680-57 | |
| Right ascension | 14h 26m 45.836397s[3] |
| Declination | −05° 10′ 19.427938″[3] |
| Apparent magnitude (V) | 16.68±0.20[2] |
| Characteristics | |
| Spectral type | G8IV[4] + M[5] + M5.5V[6] |
| Apparent magnitude (B) | 9.620[7] |
| Apparent magnitude (J) | 7.470±0.021[7] |
| Apparent magnitude (H) | 7.160±0.042[7] |
| Apparent magnitude (K) | 7.060±0.036[7] |
| B−V color index | 0.810±0.004[7] |
| Astrometry | |
| HD 126614 A | |
| Radial velocity (Rv) | −32.897±0.0042[8] km/s |
| Proper motion (μ) | RA: −149.760±0.023 mas/yr[1] Dec.: −145.837±0.018 mas/yr[1] |
| Parallax (π) | 13.6633 ± 0.0166 mas[1] |
| Distance | 238.7 ± 0.3 ly (73.19 ± 0.09 pc) |
| Absolute magnitude (MV) | 4.52[7] |
| LP 680-57 | |
| Radial velocity (Rv) | −29.45±5.52[3] km/s |
| Proper motion (μ) | RA: −147.861±0.038 mas/yr[3] Dec.: −149.118±0.034 mas/yr[3] |
| Parallax (π) | 13.6050 ± 0.0316 mas[3] |
| Distance | 239.7 ± 0.6 ly (73.5 ± 0.2 pc) |
| Absolute magnitude (MV) | 12.02[5] |
| Orbit[9] | |
| Companion | HD 126614 B |
| Period (P) | 59.979+4.696 −5.059 yr |
| Semi-major axis (a) | 15.229+0.984 −1.094 AU |
| Eccentricity (e) | 0.056+0.017 −0.018 |
| Inclination (i) | 16.294+0.881 −0.771° |
| Longitude of the node (Ω) | 284.664+2.600 −3.304° |
| Periastron epoch (T) | 2450124.747+26.090 −28.486 |
| Argument of periastron (ω) (secondary) | 240.567+30.578 −43.150° |
| Semi-amplitude (K1) (primary) | 0.167573+0.012902 −0.011124 km/s |
| Details | |
| HD 126614 A | |
| Mass | 1.145±0.03[5] M☉ |
| Radius | 1.09±0.06[5] R☉ |
| Luminosity | 1.21±0.19[5] L☉ |
| Surface gravity (log g) | 4.39±0.08[5] cgs |
| Temperature | 5,585±44[5] K |
| Metallicity | +0.56±0.04[5] |
| Rotation | ~99 days[5] |
| Rotational velocity (v sin i) | 2.0±0.5[5] km/s |
| Age | 7.2±2.0[5] Gyr |
| HD 126614 B | |
| Mass | 81.128+7.778 −7.922[9] MJup |
| LP 680-57 | |
| Mass | 0.32[10][11] M☉ |
| Radius | 0.32[10][11] R☉ |
| Luminosity | 0.0106[10] L☉ |
| Surface gravity (log g) | 4.93[10] cgs |
| Temperature | 3,275[10][11] K |
| Metallicity [Fe/H] | +0.46[6] dex |
| Age | 3.6 – 6.0[6] Gyr |
| Other designations | |
| HD 126614 AB: BD–04°3690, HD 126614, HIP 70623, SAO 139932, PPM 197558, G 124-40, LTT 5698, NLTT 37355[12] | |
| LP 680-57: LP 680-57, NLTT 37349[13] | |
| Database references | |
| SIMBAD | A |
| C | |
| Exoplanet Archive | data |
Stellar system
editHD 126614 A
editThe primary is a late G-type star with a stellar classification of G8IV.[4] It is a super metal-rich star; among the most metal-rich stars currently known.[15] This is most likely an evolving subgiant star, but the very high metallicity makes comparisons to standard spectral types difficult.[16]
HD 126614 C
editIn 2010, a close stellar companion was resolved and designated component C. This object is a faint red dwarf at an angular separation of 0.5″, which corresponds to a projected physical separation of ~ 36 AU.[16] More recent observations using radial velocity and astrometry have refined the parameters of HD 126614 C. It has an orbital period of about 60 years, with a smaller semi-major axis of 15 AU and a very low mass of 81.1 MJ.[9] This mass is very near the mass limit allowed for hydrogen fusion.
HD 126614 B
editThe outer companion, designated LP 680-57, was first reported in 1960 with the W. J. Luyten proper motion catalog.[17] It is a magnitude 17.0 red dwarf with a class of M5.5,[6] located at an angular separation of 41.90″ from the primary along a position angle of 299°, as of 2015.[17] They have a physical projected separation of 3,040 AU.[6] The common proper motion of the system has been confirmed, indicating that they are gravitationally bound.[16] Many multiple star catalogues still refer to this companion as component B, as it was known prior to the discovery of the closer companion.[17]
Planetary system
editA Doppler search for giant planets begun in 1997 at the Keck Observatory provided an 11 year baseline for detecting periodicity in the primary star's radial velocity data. In 2010, a Jovian companion was announced with an orbital period of 3.41 years.[5] In 2022, the inclination and true mass of HD 126614 Ab were measured via astrometry.[9]
| Companion (in order from star) |
Mass | Semimajor axis (AU) |
Orbital period (years) |
Eccentricity | Inclination | Radius |
|---|---|---|---|---|---|---|
| b | 0.339+0.204 −0.019 MJ |
2.249+0.088 −0.096 |
3.442+0.016 −0.017 |
0.548+0.063 −0.062 |
97.477+35.340 −37.849° |
— |
See also
editReferences
edit- ^ a b c d e Vallenari, A.; et al. (Gaia collaboration) (2023). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy and Astrophysics. 674: A1. arXiv:2208.00211. Bibcode:2023A&A...674A...1G. doi:10.1051/0004-6361/202243940. S2CID 244398875. Gaia DR3 record for this source at VizieR.
- ^ a b "HD 126614". NASA Exoplanet Archive. Retrieved 30 August 2022.
- ^ a b c d e Vallenari, A.; et al. (Gaia collaboration) (2023). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy and Astrophysics. 674: A1. arXiv:2208.00211. Bibcode:2023A&A...674A...1G. doi:10.1051/0004-6361/202243940. S2CID 244398875. Gaia DR3 record for this source at VizieR.
- ^ a b Houk, N.; Swift, C. (1999). "Michigan catalogue of two-dimensional spectral types for the HD Stars". Michigan Spectral Survey. 5. Bibcode:1999MSS...C05....0H.
- ^ a b c d e f g h i j k l Howard, Andrew W.; et al. (2010). "The California Planet Survey. I. Four New Giant Exoplanets". The Astrophysical Journal. 721 (2): 1467–1481. arXiv:1003.3488. Bibcode:2010ApJ...721.1467H. doi:10.1088/0004-637X/721/2/1467. S2CID 14147776.
- ^ a b c d e Deacon, Niall R.; et al. (2014). "Wide Cool and Ultracool Companions to Nearby Stars from Pan-STARRS 1". The Astrophysical Journal. 792 (2). 119. arXiv:1407.2938. Bibcode:2014ApJ...792..119D. doi:10.1088/0004-637X/792/2/119. S2CID 38354181.
- ^ a b c d e f g Anderson, E.; Francis, Ch. (2012). "XHIP: An extended hipparcos compilation". Astronomy Letters. 38 (5): 331. arXiv:1108.4971. Bibcode:2012AstL...38..331A. doi:10.1134/S1063773712050015. S2CID 119257644.
- ^ a b Soubiran, C.; et al. (2018). "Gaia Data Release 2. The catalogue of radial velocity standard stars". Astronomy and Astrophysics. 616: A7. arXiv:1804.09370. Bibcode:2018A&A...616A...7S. doi:10.1051/0004-6361/201832795. S2CID 52952408.
- ^ a b c d e Feng, Fabo; Butler, R. Paul; et al. (August 2022). "3D Selection of 167 Substellar Companions to Nearby Stars". The Astrophysical Journal Supplement Series. 262 (21): 21. arXiv:2208.12720. Bibcode:2022ApJS..262...21F. doi:10.3847/1538-4365/ac7e57. S2CID 251864022.
- ^ a b c d e Stassun, Keivan G.; Oelkers, Ryan J.; Pepper, Joshua; Paegert, Martin; De Lee, Nathan; Torres, Guillermo; Latham, David W.; Charpinet, Stéphane; Dressing, Courtney D.; Huber, Daniel; Kane, Stephen R.; Lépine, Sébastien; Mann, Andrew; Muirhead, Philip S.; Rojas-Ayala, Bárbara; Silvotti, Roberto; Fleming, Scott W.; Levine, Al; Plavchan, Peter; the TESS Target Selection Working Group (2018). "The TESS Input Catalog and Candidate Target List". The Astronomical Journal. 156 (3): 102. arXiv:1706.00495. Bibcode:2018AJ....156..102S. doi:10.3847/1538-3881/aad050. S2CID 73582386.
- ^ a b c Muirhead, Philip S.; Dressing, Courtney D.; Mann, Andrew W.; Rojas-Ayala, Bárbara; Lépine, Sébastien; Paegert, Martin; De Lee, Nathan; Oelkers, Ryan (2018). "A Catalog of Cool Dwarf Targets for the Transiting Exoplanet Survey Satellite". The Astronomical Journal. 155 (4): 180. arXiv:1710.00193. Bibcode:2018AJ....155..180M. doi:10.3847/1538-3881/aab710. S2CID 119184794.
- ^ a b "HD 126614". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2021-10-10.
- ^ "LP 680-57". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2022-08-30.
- ^ Busetti, F.; et al. (November 2018). "Stability of planets in triple star systems". Astronomy & Astrophysics. 619: 12. arXiv:1811.08221. Bibcode:2018A&A...619A..91B. doi:10.1051/0004-6361/201833097. S2CID 119477324. A91.
- ^ Castro, Sandra; et al. (July 1997). "High-Resolution Abundance Analysis of Very Metal-rich Stars in the Solar Neighborhood". Astronomical Journal. 114: 376–387. arXiv:astro-ph/9704220. Bibcode:1997AJ....114..376C. doi:10.1086/118481. S2CID 119368399.
- ^ a b c Lodieu, N.; et al. (September 2014). "Binary frequency of planet-host stars at wide separations. A new brown dwarf companion to a planet-host star". Astronomy & Astrophysics. 569: 14. arXiv:1408.1208. Bibcode:2014A&A...569A.120L. doi:10.1051/0004-6361/201424210. S2CID 118516214. A120.
- ^ a b c Mason, B. D.; et al. (2014). "The Washington Visual Double Star Catalog". The Astronomical Journal. 122 (6): 3466–3471. Bibcode:2001AJ....122.3466M. doi:10.1086/323920.