Omicron Aurigae
  | |
| Observation data Epoch J2000.0 Equinox J2000.0 (ICRS) | |
|---|---|
| Constellation | Auriga[1] |
| Right ascension | 05h 45m 54.042s[2] |
| Declination | +49° 49′ 34.58″[2] |
| Apparent magnitude (V) | +5.47[3] |
| Characteristics | |
| Spectral type | A1 Cr Eu[4] |
| U−B color index | +0.02 |
| B−V color index | +0.02[5] |
| Astrometry | |
| Radial velocity (Rv) | −7.7±0.9[6] km/s |
| Proper motion (μ) | RA: −11.087 mas/yr[2] Dec.: +3.703 mas/yr[2] |
| Parallax (π) | 8.1876±0.2643 mas[2] |
| Distance | 400 ± 10 ly (122 ± 4 pc) |
| Absolute magnitude (MV) | −0.03[1] |
| Details | |
| Mass | 1.9[7] M☉ |
| Radius | 3.2[7] R☉ |
| Luminosity | 50[7] L☉ |
| Surface gravity (log g) | 3.7[7] cgs |
| Temperature | 8,300[7] K |
| Rotational velocity (v sin i) | 35.2±5.3[7] km/s |
| Age | 657[8] Myr |
| Other designations | |
| ο Aur, 27 Aur, BD+49°1398, FK5 216, HD 38104, HIP 27196, HR 1971, SAO 40583[9] | |
| Database references | |
| SIMBAD | data |
Omicron Aurigae is an astrometric binary[10] star system in the northern constellation of Auriga. Its name is a Bayer designation that is Latinized from ο Aurigae, and abbreviated Omicron Aur or ο Aur. With an apparent visual magnitude of 5.47,[3] it is faintly visible to the naked eye. Based upon an annual parallax shift of 8.19 mas,[2] it is approximately 400 light-years (120 parsecs) distant from Earth. It is drifting closer to the Sun with a radial velocity of −8 km/s.[6] The star is a member of the Ursa Major stream of co-moving stars.[11]
The visible component is a chemically peculiar star with a stellar classification of A1 Cr Eu; meaning this is an A-type star with a spectrum that shows anomalously high abundances of chromium (Cr) and europium (Eu).[4] A magnetic field has been detected and it is a source of X-ray emission with a luminosity of: log Lx = 29.1.[11] The star has 1.9 times the mass of the Sun and 3.2 times the Sun's radius. It is spinning with a projected rotational velocity of 35 km/s and is radiating 50 times the Sun's luminosity from its photosphere at an effective temperature of 8,300 K.[7]
References
[edit]- 1 2 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. XHIP record for this object at VizieR.
- 1 2 3 4 5 6 Vallenari, A.; et al. (Gaia collaboration) (2023), "Gaia Data Release 3. Summary of the content and survey properties", Astronomy and Astrophysics, 674: A1, arXiv:2208.00211, Bibcode:2023A&A...674A...1G, doi:10.1051/0004-6361/202243940, S2CID 244398875. Gaia DR3 record for this source at VizieR.
- 1 2 Johnson, H. L.; et al. (1966), "UBVRIJKL photometry of the bright stars", Communications of the Lunar and Planetary Laboratory, 4 (99): 99, Bibcode:1966CoLPL...4...99J.
- 1 2 Renson, P.; Manfroid, J. (May 2009), "Catalogue of Ap, HgMn and Am stars", Astronomy and Astrophysics, 498 (3): 961–966, Bibcode:2009A&A...498..961R, doi:10.1051/0004-6361/200810788.
- ↑ Deutschman, W. A.; et al. (February 1976), "The galactic distribution of interstellar absorption as determined from the Celescope catalog of ultraviolet stellar observations and a new catalogue of UBV, Hbeta photoelectric observations", Astrophysical Journal Supplement Series, 30: 97–225, Bibcode:1976ApJS...30...97D, doi:10.1086/190359.
- 1 2 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.
- 1 2 3 4 5 6 7 Moiseeva, A. V.; et al. (January 2019), "Fundamental Parameters of CP Stars Observed at the 6-m Telescope. I. Observations in 2009–2011", Astrophysical Bulletin, 74 (1): 62–65, Bibcode:2019AstBu..74...62M, doi:10.1134/S1990341319010061.
- ↑ Kordopatis, G.; Schultheis, M.; McMillan, P. J.; Palicio, P. A.; De Laverny, P.; Recio-Blanco, A.; Creevey, O.; Álvarez, M. A.; Andrae, R.; Poggio, E.; Spitoni, E.; Contursi, G.; Zhao, H.; Oreshina-Slezak, I.; Ordenovic, C.; Bijaoui, A. (2023). "Stellar ages, masses, extinctions, and orbital parameters based on spectroscopic parameters of Gaia DR3". Astronomy and Astrophysics. 669: A104. arXiv:2206.07937. Bibcode:2023A&A...669A.104K. doi:10.1051/0004-6361/202244283.
- ↑ "omi Aur". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2017-06-28.
- ↑ Makarov, V. V.; Kaplan, G. H. (May 2005), "Statistical Constraints for Astrometric Binaries with Nonlinear Motion", The Astronomical Journal, 129 (5): 2420–2427, Bibcode:2005AJ....129.2420M, doi:10.1086/429590.
- 1 2 Panzera, M. R.; et al. (August 1999), "X-ray emission from A0-F6 spectral type stars", Astronomy and Astrophysics, 348: 161–169, arXiv:astro-ph/9906221, Bibcode:1999A&A...348..161P.
