Summary
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 edit
HD 126614 A edit
The 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 edit
In 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 edit
The 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 edit
A 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 edit
References 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.