| Observation data Epoch J2000.0 Equinox J2000.0 (ICRS) | |
|---|---|
| Constellation | Taurus |
| Right ascension | 04h 17m 15.66155s[1] |
| Declination | +20° 34′ 42.9340″[1] |
| Apparent magnitude (V) | +4.914[2] |
| Characteristics | |
| Spectral type | A3m[3] |
| B−V color index | +0.259[4] |
| Astrometry | |
| Radial velocity (Rv) | +15.0±0.6[5] km/s |
| Proper motion (μ) | RA: −39.41[1] mas/yr Dec.: −60.79[1] mas/yr |
| Parallax (π) | 34.55 ± 0.38 mas[1] |
| Distance | 94 ± 1 ly (28.9 ± 0.3 pc) |
| Absolute magnitude (MV) | +2.62[6] |
| Details | |
| Mass | 1.9±0.1[3] M☉ |
| Radius | 1.514±0.044[7] R☉ |
| Luminosity | 6.6[8] L☉ |
| Temperature | 7,541±137[7] K |
| Rotational velocity (v sin i) | 70.1[4] km/s |
| Age | 100[4] Myr |
| Other designations | |
| Database references | |
| SIMBAD | data |
Omega2 Tauri is a solitary,[10] white hued star in the zodiac constellation of Taurus. It has an apparent visual magnitude of +4.9,[2] which is bright enough to be seen with the naked eye at night. The distance to this system, as determined using an annual parallax shift of 34.55 mas as seen from the Earth,[1] is about 94 light years.
This is a young Am star with an age of around 100 million[4] years and a stellar classification of A3m.[3] It displays an infrared excess emission, indicating the presence of an orbiting debris disk with a mean temperature of 99 K.[11] This star is a probable member of the Octans Near association, a nearby moving group of stars that share a common motion through space.[4]
References
- ^ a b c d e f 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.
- ^ a b Høg, E.; et al. (2000), "The Tycho-2 catalogue of the 2.5 million brightest stars", Astronomy and Astrophysics, 355: L27, Bibcode:2000A&A...355L..27H.
- ^ a b c Tetzlaff, N.; et al. (January 2011), "A catalogue of young runaway Hipparcos stars within 3 kpc from the Sun", Monthly Notices of the Royal Astronomical Society, 410 (1): 190–200, arXiv:1007.4883, Bibcode:2011MNRAS.410..190T, doi:10.1111/j.1365-2966.2010.17434.x, S2CID 118629873.
- ^ a b c d e Zuckerman, B.; et al. (November 2013), "Young Stars near Earth: The Octans-Near Association and Castor Moving Group", The Astrophysical Journal, 778 (1): 12, arXiv:1309.2318, Bibcode:2013ApJ...778....5Z, doi:10.1088/0004-637X/778/1/5, S2CID 118446756, 5.
- ^ de Bruijne, J. H. J.; Eilers, A.-C. (October 2012), "Radial velocities for the HIPPARCOS-Gaia Hundred-Thousand-Proper-Motion project", Astronomy & Astrophysics, 546: 14, arXiv:1208.3048, Bibcode:2012A&A...546A..61D, doi:10.1051/0004-6361/201219219, S2CID 59451347, A61.
- ^ 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 Masana, E.; et al. (2006), "Effective temperature scale and bolometric corrections from 2MASS photometry", Astronomy and Astrophysics, 450 (2): 735, arXiv:astro-ph/0601049, Bibcode:2006A&A...450..735M, doi:10.1051/0004-6361:20054021, S2CID 15278668.
- ^ McDonald, I.; et al. (2012), "Fundamental Parameters and Infrared Excesses of Hipparcos Stars", Monthly Notices of the Royal Astronomical Society, 427 (1): 343–57, arXiv:1208.2037, Bibcode:2012MNRAS.427..343M, doi:10.1111/j.1365-2966.2012.21873.x, S2CID 118665352.
- ^ "ome02 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.
- ^ Su, K. Y. L.; et al. (December 2006), "Debris Disk Evolution around A Stars", The Astrophysical Journal, 653 (1): 675–689, arXiv:astro-ph/0608563, Bibcode:2006ApJ...653..675S, doi:10.1086/508649, S2CID 14116473.
This page was last edited on 27 March 2022, at 05:38