Astronomy:Omega1 Tauri
| Observation data Equinox J2000.0]] (ICRS) | |
|---|---|
| Constellation | Taurus |
| Right ascension | 02h 12m 22.28003s[1] |
| Declination | +30° 18′ 11.0430″[1] |
| Apparent magnitude (V) | +5.51[2] |
| Characteristics | |
| Spectral type | K2 III[2] |
| B−V color index | 1.077[2] |
| Astrometry | |
| Radial velocity (Rv) | +24.75±0.02[2] km/s |
| Proper motion (μ) | RA: −65.05[1] mas/yr Dec.: −60.50[1] mas/yr |
| Parallax (π) | 11.22 ± 0.70[1] mas |
| Distance | 290 ± 20 ly (89 ± 6 pc) |
| Absolute magnitude (MV) | +0.76[2] |
| Details | |
| Mass | 1.53[3] M☉ |
| Radius | 12[4] R☉ |
| Luminosity | 57.5[3] L☉ |
| Surface gravity (log g) | 2.5[5] cgs |
| Temperature | 4,737±77[3] K |
| Metallicity [Fe/H] | 0.12[5] dex |
| Rotational velocity (v sin i) | 4.6[4] km/s |
| Age | 4.21[3] Gyr |
| Other designations | |
| Database references | |
| SIMBAD | data |
Omega1 Tauri is a solitary,[7] 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.[2] Based upon an annual parallax shift of 11.22 mas as seen from Earth,[1] 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.[2] At the estimated age of 4.2 billion years,[3] it is a red clump star that is generating energy by helium fusion at its core.[5] Omega1 Tauri has about 1.5[3] times the mass of the Sun and has expanded to around 12[4] 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.[3] The radial velocity of this star shows no appreciable variation, and for this reason it is used as a radial velocity standard.[2]
References
- ↑ 1.0 1.1 1.2 1.3 1.4 1.5 van Leeuwen, F. (2007), "Validation of the new Hipparcos reduction", Astronomy and Astrophysics 474 (2): 653–664, doi:10.1051/0004-6361:20078357, Bibcode: 2007A&A...474..653V.
- ↑ 2.0 2.1 2.2 2.3 2.4 2.5 2.6 2.7 Hekker, S. et al. (August 2006), "Precise radial velocities of giant stars. I. Stable stars", Astronomy and Astrophysics 454 (3): 943–949, doi:10.1051/0004-6361:20064946, Bibcode: 2006A&A...454..943H.
- ↑ 3.0 3.1 3.2 3.3 3.4 3.5 3.6 Luck, R. Earle (2015), "Abundances in the Local Region. I. G and K Giants", Astronomical Journal 150 (3): 88, doi:10.1088/0004-6256/150/3/88, Bibcode: 2015AJ....150...88L.
- ↑ 4.0 4.1 4.2 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, doi:10.1088/0004-6256/135/1/209, Bibcode: 2008AJ....135..209M.
- ↑ 5.0 5.1 5.2 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, doi:10.1093/mnras/sts663, Bibcode: 2013MNRAS.430..621T.
- ↑ "ome01 Tau". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=ome01+Tau.
- ↑ 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, doi:10.1111/j.1365-2966.2008.13596.x, Bibcode: 2008MNRAS.389..869E.
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