Omega Aurigae

Omega Aurigae
Location of ω Aurigae (circled in red)
Observation data
Epoch J2000      Equinox ICRS
Constellation Auriga
Right ascension 04h 59m 15.409s
Declination +37° 53′ 24.88″
Apparent magnitude (V) 4.95
Characteristics
Evolutionary stage main sequence
Spectral type A1 V
U−B color index +0.01
B−V color index +0.05
R−I color index 0.03
Astrometry
Radial velocity (Rv)+7.7±2.5 km/s
Proper motion (μ) RA: +45.340 mas/yr
Dec.: −97.647 mas/yr
Parallax (π)20.1236±0.2385 mas
Distance162 ± 2 ly
(49.7 ± 0.6 pc)
Absolute magnitude (MV)+1.34
Details
ω Aur A
Mass2.29±0.04 M☉
Radius2.0 R☉
Luminosity27 L☉
Surface gravity (log g)4.33 cgs
Temperature9,230 K
Metallicity [Fe/H]−0.12 dex
Rotational velocity (v sin i)107 km/s
Age317 Myr
ω Aur B
Mass1.1 M☉
Other designations
ω Aur, 4 Aur, BD+37°1005, GC 6064, HD 31647, HIP 23179, HR 1592, SAO 57548, PPM 400070, WDS J04593+3753AB
Database references
SIMBADdata

Omega Aurigae is a double star 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, 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). It is receding from the Sun with a radial velocity of +8 km/s. The system is a member of the Columba group of co-moving stars.

The primary component is an A-type main sequence star with a stellar classification of A1 V. It is 317 million years old with a high rate of spin, showing a projected rotational velocity of 107 km/s. The star has 2.3 times the mass of the Sun and double the Sun's radius. It is radiating 27 times the Sun's luminosity from its photosphere at an effective temperature of 9,230 K. The object displays an infrared excess, suggesting an orbiting debris disk with a temperature of 20 K at a mean radius of 932.40 AU from the host star.

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. The system is an X-ray source with a luminosity of 16.57×1029 ergs s−1.

References

  1. 1 2 3 4 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.
  2. 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.
  3. 1 2 3 4 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. 1 2 3 Zorec, J.; Royer, F. (2012), "Rotational velocities of A-type stars. IV. Evolution of rotational velocities", Astronomy & Astrophysics, 537: A120, arXiv:1201.2052, Bibcode:2012A&A...537A.120Z, doi:10.1051/0004-6361/201117691, S2CID 55586789.
  5. 1 2 3 4 5 6 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. 1 2 Gontcharov, G. A. (2006), "Pulkovo compilation of radial velocities for 35495 stars in a common system", Astronomy Letters, 32 (11): 759–771, arXiv:1606.08053, Bibcode:2006AstL...32..759G, doi:10.1134/S1063773706110065, S2CID 119231169.
  7. 1 2 3 Cotten, Tara H.; Song, Inseok (July 2016), "A Comprehensive Census of Nearby Infrared Excess Stars", The Astrophysical Journal Supplement Series, 225 (1): 24, arXiv:1606.01134, Bibcode:2016ApJS..225...15C, doi:10.3847/0067-0049/225/1/15, S2CID 118438871, 15.
  8. 1 2 Royer, F.; et al. (February 2007), "Rotational velocities of A-type stars. III. Velocity distributions", Astronomy and Astrophysics, 463 (2): 671–682, arXiv:astro-ph/0610785, Bibcode:2007A&A...463..671R, doi:10.1051/0004-6361:20065224, S2CID 18475298.
  9. 1 2 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, arXiv:1501.03154, Bibcode:2015ApJ...804..146D, doi:10.1088/0004-637X/804/2/146, S2CID 33401607.
  10. 1 2 Gratton, R.; et al. (May 2024), "Stellar companions and Jupiter-like planets in young associations", Astronomy & Astrophysics, 685, id. A119, arXiv:2402.02148, Bibcode:2024A&A...685A.119G, doi:10.1051/0004-6361/202348393.
  11. ↑ "* ome Aur". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2012-08-24.
  12. ↑ 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.
  13. ↑ 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, arXiv:1604.03550, Bibcode:2016A&A...590A..13E, doi:10.1051/0004-6361/201628253, S2CID 53138126, A13.
  14. ↑ Makarov, Valeri V. (October 2003), "The 100 Brightest X-Ray Stars within 50 Parsecs of the Sun", The Astronomical Journal, 126 (4): 1996–2008, Bibcode:2003AJ....126.1996M, doi:10.1086/378164.