Astronomy:Omega Aurigae
| Observation data Equinox J2000.0]] (ICRS) | |
|---|---|
| Constellation | Auriga[1] |
| Right ascension | 04h 59m 15.409s[2] |
| Declination | +37° 53′ 24.88″[2] |
| Apparent magnitude (V) | 4.95[3] |
| Characteristics | |
| Evolutionary stage | main sequence[4] |
| Spectral type | A1 V[5] |
| U−B color index | +0.01[3] |
| B−V color index | +0.05[3] |
| R−I color index | 0.03 |
| Astrometry | |
| Radial velocity (Rv) | +7.7±2.5[6] km/s |
| Proper motion (μ) | RA: +45.340[2] mas/yr Dec.: −97.647[2] mas/yr |
| Parallax (π) | 20.1236 ± 0.2385[2] mas |
| Distance | 162 ± 2 ly (49.7 ± 0.6 pc) |
| Absolute magnitude (MV) | +1.34[1] |
| Details | |
| ω Aur A | |
| Mass | 2.29±0.04[4] M☉ |
| Radius | 2.0[7] R☉ |
| Luminosity | 27[1] L☉ |
| Surface gravity (log g) | 4.33[5] cgs |
| Temperature | 9,230[5] K |
| Metallicity [Fe/H] | −0.12[5] dex |
| Rotational velocity (v sin i) | 107[8] km/s |
| Age | 317[9] Myr |
| ω Aur B | |
| Mass | 1.1[10] M☉ |
| Other designations | |
| Database references | |
| SIMBAD | data |
Omega Aurigae is a double star[12] in the northern constellation of Auriga. Its name is a Bayer designation that is Latinized from ω Aurigae, and abbreviated Omega Aur or ω Aur. This star has a combined apparent visual magnitude of 4.95,[3] which is bright enough to be seen with the naked eye. The distance to this system, as determined using parallax measurements, is approximately 162 light-years (50 parsecs).[2] It is receding from the Sun with a radial velocity of +8 km/s.[6] The system is a member of the Columba group of co-moving stars.[13]
The primary component is an A-type main sequence star with a stellar classification of A1 V.[5] It is 317[9] million years old with a high rate of spin, showing a projected rotational velocity of 107 km/s.[8] The star has 2.3[4] times the mass of the Sun and double[7] the Sun's radius. It is radiating 27[1] times the Sun's luminosity from its photosphere at an effective temperature of 9,230 K.[5] The object displays an infrared excess, suggesting an orbiting debris disk with a temperature of 20 K at a mean radius of 932.40 astronomical unit|AU from the host star.[7]
There is a magnitude 8.18 companion at an angular separation of 4.99 arcseconds along a position angle of 4.30°. This corresponds to a physical separation of 234.2 au.[10] The system is an X-ray source with a luminosity of 16.57×1029 ergs s−1.[14]
References
- ↑ 1.0 1.1 1.2 1.3 Anderson, E.; Francis, Ch. (2012). "XHIP: An extended hipparcos compilation". Astronomy Letters 38 (5): 331. doi:10.1134/S1063773712050015. Bibcode: 2012AstL...38..331A. XHIP record for this object at VizieR.
- ↑ 2.0 2.1 2.2 2.3 2.4 Vallenari, A. et al. (2022). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy & Astrophysics. doi:10.1051/0004-6361/202243940. Gaia DR3 record for this source at VizieR.
- ↑ 3.0 3.1 3.2 3.3 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.
- ↑ 4.0 4.1 4.2 Zorec, J.; Royer, F. (2012), "Rotational velocities of A-type stars. IV. Evolution of rotational velocities", Astronomy & Astrophysics 537: A120, doi:10.1051/0004-6361/201117691, Bibcode: 2012A&A...537A.120Z.
- ↑ 5.0 5.1 5.2 5.3 5.4 5.5 Hill, G. M. (February 1995), "Compositional differences among the A-type stars. 2: Spectrum synthesis up to V sin i = 110 km/s", Astronomy and Astrophysics 294 (2): 536–546, Bibcode: 1995A&A...294..536H.
- ↑ 6.0 6.1 Gontcharov, G. A. (2006), "Pulkovo compilation of radial velocities for 35495 stars in a common system", Astronomy Letters 32 (11): 759–771, doi:10.1134/S1063773706110065, Bibcode: 2006AstL...32..759G.
- ↑ 7.0 7.1 7.2 Cotten, Tara H.; Song, Inseok (July 2016), "A Comprehensive Census of Nearby Infrared Excess Stars", The Astrophysical Journal Supplement Series 225 (1): 24, doi:10.3847/0067-0049/225/1/15, 15, Bibcode: 2016ApJS..225...15C.
- ↑ 8.0 8.1 Royer, F. et al. (February 2007), "Rotational velocities of A-type stars. III. Velocity distributions", Astronomy and Astrophysics 463 (2): 671–682, doi:10.1051/0004-6361:20065224, Bibcode: 2007A&A...463..671R.
- ↑ 9.0 9.1 David, Trevor J.; Hillenbrand, Lynne A. (2015), "The Ages of Early-Type Stars: Strömgren Photometric Methods Calibrated, Validated, Tested, and Applied to Hosts and Prospective Hosts of Directly Imaged Exoplanets", The Astrophysical Journal 804 (2): 146, doi:10.1088/0004-637X/804/2/146, Bibcode: 2015ApJ...804..146D.
- ↑ 10.0 10.1
- ↑ "* ome Aur". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=%2A+ome+Aur.
- ↑ 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.
- ↑ Elliott, P. et al. (May 2016), "Search for associations containing young stars (SACY). VII. New stellar and substellar candidate members in the young associations", Astronomy & Astrophysics 590: 28, doi:10.1051/0004-6361/201628253, A13, Bibcode: 2016A&A...590A..13E.
- ↑ Makarov, Valeri V. (October 2003), "The 100 Brightest X-Ray Stars within 50 Parsecs of the Sun", The Astronomical Journal 126 (4): 1996–2008, doi:10.1086/378164, Bibcode: 2003AJ....126.1996M.
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