Omicron Virginis
 
| |
| Observation data Epoch J2000.0 Equinox J2000.0 | |
|---|---|
| Constellation | Virgo |
| Right ascension | 12h 05m 12.54049s[1] |
| Declination | +08° 43′ 58.7498″[1] |
| Apparent magnitude (V) | 4.12[2] |
| Characteristics | |
| Spectral type | G8 IIIa CN-1Ba1CH1[3] |
| Astrometry | |
| Radial velocity (Rv) | −29.62[4] km/s |
| Proper motion (μ) | RA: −218.69[1] mas/yr Dec.: +57.76[1] mas/yr |
| Parallax (π) | 19.98 ± 0.22[1] mas |
| Distance | 163 ± 2 ly (50.1 ± 0.6 pc) |
| Absolute magnitude (MV) | +0.52[5] |
| Details[4] | |
| Mass | 2.17 M☉ |
| Radius | 9.62 R☉ |
| Luminosity | 57 L☉ |
| Surface gravity (log g) | 3.17 cgs |
| Temperature | 5,107 K |
| Metallicity [Fe/H] | −0.30 dex |
| Rotational velocity (v sin i) | 2.23 km/s |
| Age | 0.88 Gyr |
| Other designations | |
| Database references | |
| SIMBAD | data |
Omicron Virginis (ο Vir, ο Virginis) is a star in the zodiac constellation of Virgo. It is visible to the naked eye with an apparent visual magnitude of +4.12.[5] Based upon parallax measurements, it is about 163 light years from the Sun.
ο Virginis is a G-type giant star with a stellar classification of G8 IIIa CN-1Ba1CH1.[3] This indicates that it is a Barium star. Typically Barium stars are close binaries with a white dwarf companion, but no companion ihas been detected for ο Virginis.[6] It has been suggested that an excess SiIV emission flux is due to an unseen white dwarf companion.[7]
ο Virginis is a giant star around tens times larger than the sun. Although it is slightly cooler, it is radiating about 60-132 times the luminosity of the Sun. It is over twice as massive as the sun and is around a billion years old.[5][4] A simplified statistical analysis suggests that ο Virginis is likely to be a red giant branch star fusing hydrogen in a shell around an inert helium core, but there is about a 22% chance that it is a horizontal branch star fusing helium in its core.[8]
References
- 1 2 3 4 5 van Leeuwen, F. (2007), "Validation of the new Hipparcos reduction", Astronomy and Astrophysics, 474 (2): 653–664, arXiv:0708.1752
, Bibcode:2007A&A...474..653V, doi:10.1051/0004-6361:20078357. - ↑ Mallik, Sushma V. (December 1999), "Lithium abundance and mass", Astronomy and Astrophysics, 352: 495–507, Bibcode:1999A&A...352..495M.
- 1 2 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.
- 1 2 3 Jofré, E.; Petrucci, R.; Saffe, C.; Saker, L.; de la Villarmois, E. Artur; Chavero, C.; Gómez, M.; Mauas, P. J. D. (2015). "Stellar parameters and chemical abundances of 223 evolved stars with and without planets". Astronomy & Astrophysics. 574: A50. Bibcode:2015A&A...574A..50J. doi:10.1051/0004-6361/201424474.
- 1 2 3 Takeda, Yoichi; et al. (August 2008), "Stellar Parameters and Elemental Abundances of Late-G Giants", Publications of the Astronomical Society of Japan, 60 (4): 781–802, arXiv:0805.2434, Bibcode:2008PASJ...60..781T, doi:10.1093/pasj/60.4.781.
- ↑ Začs, Laimons (2000). "The Chemical Composition and Orbital Parameters of Barium Stars". The Carbon Star Phenomenon. 177: 277. Bibcode:2000IAUS..177..277Z.
- ↑ Böhm-Vitense, Erika; Carpenter, Kenneth; Robinson, Richard; Ake, Tom; Brown, Jeffery (2000). "Do All BA II Stars Have White Dwarf Companions?". The Astrophysical Journal. 533 (2): 969. Bibcode:2000ApJ...533..969B. doi:10.1086/308678.
- ↑ Reffert, Sabine; Bergmann, Christoph; Quirrenbach, Andreas; Trifonov, Trifon; Künstler, Andreas (2015). "Precise radial velocities of giant stars. VII. Occurrence rate of giant extrasolar planets as a function of mass and metallicity". Astronomy & Astrophysics. 574: A116. Bibcode:2015A&A...574A.116R. doi:10.1051/0004-6361/201322360.