HD 106760 is a single-lined spectroscopic binary[8] star system in the northern constellation of Coma Berenices. It is faintly visible to the naked eye, having an apparent visual magnitude of 4.99.[2] The system is located around 318 light years away, as determined from its annual parallax shift of 10.2417 mas.[1] It is moving closer with a heliocentric radial velocity of −40 km/s, and is expected to come as close as 259 ly in about 772,000 years.[2]
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Coma Berenices |
| Right ascension | 12h 16m 30.12328s[1] |
| Declination | +33° 03′ 41.4198″[1] |
| Apparent magnitude (V) | 4.99[2] |
| Characteristics | |
| Spectral type | K0.5 III–IIIb[3] |
| B−V color index | 1.140±0.002[2] |
| Astrometry | |
| Radial velocity (Rv) | −40.4±0.3[2] km/s |
| Proper motion (μ) | RA: −41.979[1] mas/yr Dec.: −105.115[1] mas/yr |
| Parallax (π) | 10.2417 ± 0.2354 mas[1] |
| Distance | 318 ± 7 ly (98 ± 2 pc) |
| Absolute magnitude (MV) | 0.06[2] |
| Orbit[4] | |
| Period (P) | 3.598 years (1,314.3 d) |
| Eccentricity (e) | 0.43 |
| Longitude of the node (Ω) | 303.6° |
| Periastron epoch (T) | 2441468.5 JD |
| Semi-amplitude (K1) (primary) | 6.5 km/s |
| Details[5] | |
| Mass | 1.85±0.14 M☉ |
| Radius | 16.79±0.79 R☉ |
| Luminosity | 112[6] L☉ |
| Surface gravity (log g) | 2.48±0.10 cgs |
| Temperature | 4,581±28 K |
| Metallicity [Fe/H] | −0.12±0.05 dex |
| Rotational velocity (v sin i) | 0.9[6] km/s |
| Age | 1.57±0.32 Gyr |
| Other designations | |
| Database references | |
| SIMBAD | data |
The variable radial velocity of HD 106760 was announced by W. W. Campbell of Lick Observatory in 1922, indicating the binary nature of this system. A preliminary orbit was determined by Mount Wilson Observatory astronomer W. H. Christie in 1936, then refined by English astronomer R. F. Griffin in 1984.[8] The components of this system orbit each other with a period of 3.6 years and an eccentricity of 0.43.[4]
The visible component has a stellar classification of K0.5 III–IIIb,[3] indicating it is an evolved K-type giant star. It is around 1.6 billion years old with 1.9 times the mass of the Sun and has expanded to 17 times the Sun's radius.[5] The star is radiating 112[6] times the Sun's luminosity from its enlarged photosphere at an effective temperature of 4,581 K.[5]
References
edit- ^ a b c d e f Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics. 616. A1. arXiv:1804.09365. Bibcode:2018A&A...616A...1G. doi:10.1051/0004-6361/201833051.
- ^ a b c d e f 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 Keenan, Philip C.; McNeil, Raymond C. (1989), "The Perkins catalog of revised MK types for the cooler stars", Astrophysical Journal Supplement Series, 71: 245, Bibcode:1989ApJS...71..245K, doi:10.1086/191373
- ^ a b Pourbaix, D.; et al. (2004), "SB9: The Ninth Catalogue of Spectroscopic Binary Orbits", Astronomy & Astrophysics, 424: 727–732, arXiv:astro-ph/0406573, Bibcode:2004A&A...424..727P, doi:10.1051/0004-6361:20041213, S2CID 119387088.
- ^ a b c Maldonado, J.; Villaver, E. (April 2016), "Evolved stars and the origin of abundance trends in planet hosts", Astronomy & Astrophysics, 588: 11, arXiv:1602.00835, Bibcode:2016A&A...588A..98M, doi:10.1051/0004-6361/201527883, S2CID 119212009, A98.
- ^ a b c Massarotti, Alessandro; et al. (January 2008), "Rotational and Radial Velocities for a Sample of 761 HIPPARCOS Giants and the Role of Binarity", The Astronomical Journal, 135 (1): 209–231, Bibcode:2008AJ....135..209M, doi:10.1088/0004-6256/135/1/209, S2CID 121883397.
- ^ "HD 106760". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2018-07-13.
- ^ a b Griffin, R. F. (June 1984), "Spectroscopic binaries near the North Galactic Pole. X - HR 4668", Journal of Astrophysics and Astronomy, 5: 181−185, Bibcode:1984JApA....5..181G, doi:10.1007/BF02714990, S2CID 124007568.