| Observation data Epoch J2000.0 Equinox J2000.0 (ICRS) | |
|---|---|
| Constellation | Taurus |
| Right ascension | 04 07 09.97 |
| Declination | +19° 36′ 33.2″ |
| Apparent magnitude (V) | +5.51 |
| Characteristics | |
| Spectral type | K2 III |
| B−V color index | 1.077 |
| Astrometry | |
| Radial velocity (Rv) | +24.75±0.02 km/s |
| Proper motion (μ) | RA: −65.05 mas/yr Dec.: −60.50 mas/yr |
| Parallax (π) | 11.22 ± 0.70 mas |
| Distance | 290 ± 20 ly (89 ± 6 pc) |
| Absolute magnitude (MV) | +0.76 |
| Details | |
| Mass | 1.53 M☉ |
| Radius | 12 R☉ |
| Luminosity | 57.5 L☉ |
| Surface gravity (log g) | 2.5 cgs |
| Temperature | 4,737±77 K |
| Metallicity | 0.12 dex |
| Rotational velocity (v sin i) | 4.6 km/s |
| Age | 4.21 Gyr |
| Other designations | |
| ω Tau, 43 Tau, BD+19° 672, FK5 1115, HD 26162, HIP 19388, HR 1283, SAO 93785 | |
| Database references | |
| SIMBAD | data |
Omega Tauri is a solitary, orange hued star in the zodiac constellation of Taurus. It is faintly visible to the naked eye with an apparent visual magnitude of +5.51. Based upon an annual parallax shift of 11.22 mas as seen from Earth, it is located about 290 light years from the Sun.
This is an evolved K-type giant star with a stellar classification of K2 III. At the estimated age of 4.2 billion years, it is a red clump star that is generating energy by helium fusion at its core. Omega Tauri has about 1.5 times the mass of the Sun and has expanded to around 12 times the Sun's radius. It is radiating 57.5 times the Sun's luminosity from its photosphere at an effective temperature of 4,737 K. The radial velocity of this star shows no appreciable variation, and for this reason it is used as a radial velocity standard.
References
- ^ 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, S2CID 18759600.
- ^ Hekker, S.; et al. (August 2006), "Precise radial velocities of giant stars. I. Stable stars", Astronomy and Astrophysics, 454 (3): 943–949, arXiv:astro-ph/0604502, Bibcode:2006A&A...454..943H, doi:10.1051/0004-6361:20064946, S2CID 119529768.
- ^ Luck, R. Earle (2015), "Abundances in the Local Region. I. G and K Giants", Astronomical Journal, 150 (3), 88, arXiv:1507.01466, Bibcode:2015AJ....150...88L, doi:10.1088/0004-6256/150/3/88, S2CID 118505114.
- ^ 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.
- ^ Tautvaišienė, G.; et al. (March 2013), "Red clump stars of the Milky Way - laboratories of extra-mixing", Monthly Notices of the Royal Astronomical Society, 430 (1): 621−627, arXiv:1304.4393, Bibcode:2013MNRAS.430..621T, doi:10.1093/mnras/sts663, S2CID 119211439.
- "ome01 Tau". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2017-06-30.
- Eggleton, P. P.; Tokovinin, A. A. (September 2008), "A catalogue of multiplicity among bright stellar systems", Monthly Notices of the Royal Astronomical Society, 389 (2): 869–879, arXiv:0806.2878, Bibcode:2008MNRAS.389..869E, doi:10.1111/j.1365-2966.2008.13596.x, S2CID 14878976.
