HD 167665 is a yellow-white hued star with a brown dwarf companion in the southern constellation of Sagittarius. With an apparent visual magnitude of 6.39,[2] it is near the lower brightness limit for stars that are visible to the naked eye. Based upon an annual parallax shift of 32.4 mas as seen from Earth, it is located 101 light years from the Sun. The star is moving away from the Sun with a radial velocity of +8 km/s.[9]
| Observation data Epoch J2000.0 Equinox J2000.0 | |
|---|---|
| Constellation | Sagittarius |
| Right ascension | 18h 17m 23.759s[1] |
| Declination | −28° 17′ 20.22″[1] |
| Apparent magnitude (V) | 6.39[2] |
| Characteristics | |
| Spectral type | F9V Fe−0.8 CH−0.4[3] |
| U−B color index | +0.00[2] |
| B−V color index | +0.52[2] |
| Astrometry | |
| Radial velocity (Rv) | 8.41±0.23[1] km/s |
| Proper motion (μ) | RA: 133.261±0.094 mas/yr[1] Dec.: −151.806±0.065 mas/yr[1] |
| Parallax (π) | 32.3999 ± 0.0903 mas[1] |
| Distance | 100.7 ± 0.3 ly (30.86 ± 0.09 pc) |
| Absolute magnitude (MV) | +3.94[4] |
| Orbit[5] | |
| Period (P) | 12.154+0.034 −0.036 yr |
| Semi-major axis (a) | 5.618+0.236 −0.261 AU |
| Eccentricity (e) | 0.342±0.006 |
| Inclination (i) | 95.195+7.475 −9.865° |
| Longitude of the node (Ω) | 219.017+1.580 −1.410° |
| Periastron epoch (T) | 2448065.856+16.941 −16.172 |
| Argument of periastron (ω) (secondary) | 222.528+0.862 −0.893° |
| Semi-amplitude (K1) (primary) | 0.611353+0.003287 −0.003526 km/s |
| Details[6] | |
| Mass | 1.03±0.01 M☉ |
| Radius | 1.32±0.02 R☉ |
| Luminosity | 2.45[4] L☉ |
| Surface gravity (log g) | 4.13±0.03 cgs |
| Temperature | 6,080±15 K |
| Metallicity [Fe/H] | −0.21±0.01 dex |
| Rotational velocity (v sin i) | 8[7] km/s |
| Age | 6.72±0.23 Gyr |
| Other designations | |
| Database references | |
| SIMBAD | data |
This star has a stellar classification of F9V Fe−0.8 CH−0.4,[3] which indicates this is an F-type main-sequence star with a spectrum that displays mild underabundances of iron and the CH molecule compared to normal stars of this temperature. It is a solar-type star with about the same mass as the Sun, but has a radius 32% greater.[6] The star is older than the Sun with an estimated age of 6.7 billion years,[6] and it is spinning with a projected rotational velocity of 8 km/s.[7] HD 167665 is radiating 2.45[4] times the Sun's luminosity from its photosphere at an effective temperature of 6,080 K.[6]
Based upon regular variations in radial velocity observed between 1996 and 2006, an orbiting companion was announced by the California and Carnegie Planet Search (CCPS) program in 2007. This perturbing object, designated HD 167665 b,[10] has an orbital period of twelve years with an eccentricity of 0.342. The semimajor axis of this orbit is 5.62 AU[5] and the object has a mass of at least 50.3±0.4 MJ. Since the inclination of the orbit was initially unknown, the exact mass could not be determined, with a 79% chance that the mass of the object constrains it to be a brown dwarf with a mass less than 82 MJ.[11] In 2022, astrometric observations confirmed this object to be a brown dwarf, with a true mass of 52.708+5.112
−4.403 MJ. Its inclination suggests a non-zero probability that it transits its star.[5]
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 c d Stobie, R. S. (1970), "Photometry of bright southern Cepheids", Monthly Notices of the Royal Astronomical Society, 148: 1–15, Bibcode:1970MNRAS.148....1S, doi:10.1093/mnras/148.1.1.
- ^ a b Gray, R. O.; et al. (2006), "Contributions to the Nearby Stars (NStars) Project: Spectroscopy of Stars Earlier than M0 within 40 pc--The Southern Sample", The Astronomical Journal, 132 (1): 161–170, arXiv:astro-ph/0603770, Bibcode:2006AJ....132..161G, doi:10.1086/504637, S2CID 119476992.
- ^ a b c 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 c 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 Maldonado, J.; Villaver, E. (June 2017), "Searching for chemical signatures of brown dwarf formation", Astronomy & Astrophysics, 602: 15, arXiv:1702.02904, Bibcode:2017A&A...602A..38M, doi:10.1051/0004-6361/201630120, S2CID 56225222, A38.
- ^ a b Balachandran, Suchitra (May 1, 1990), "Lithium depletion and rotation in main-sequence stars", Astrophysical Journal, Part 1, 354: 310–332, Bibcode:1990ApJ...354..310B, doi:10.1086/168691.
- ^ "HD 167665". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2017-10-27.
- ^ Nordström, B.; et al. (May 2004), "The Geneva-Copenhagen survey of the Solar neighbourhood. Ages, metallicities, and kinematic properties of ˜14 000 F and G dwarfs", Astronomy and Astrophysics, 418: 989–1019, arXiv:astro-ph/0405198, Bibcode:2004A&A...418..989N, doi:10.1051/0004-6361:20035959, S2CID 11027621.
- ^ Reffert, S.; Quirrenbach, A. (March 2011), "Mass constraints on substellar companion candidates from the re-reduced Hipparcos intermediate astrometric data: nine confirmed planets and two confirmed brown dwarfs", Astronomy & Astrophysics, 527: 22, arXiv:1101.2227, Bibcode:2011A&A...527A.140R, doi:10.1051/0004-6361/201015861, S2CID 54986291, A140.
- ^ Patel, Shannon G.; et al. (August 2007), "Fourteen New Companions from the Keck and Lick Radial Velocity Survey Including Five Brown Dwarf Candidates", The Astrophysical Journal, 665 (1): 744–753, arXiv:0704.3418, Bibcode:2007ApJ...665..744P, doi:10.1086/519066, S2CID 55357942.