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Omega Aurigae

From Wikipedia, the free encyclopedia

"HR 1592" redirects here. For the legislation, see Matthew Shepard Act.
Omega Aurigae
Observation data
Epoch J2000      Equinox J2000
Constellation Auriga
Right ascension 04h 59m 15.41038s[1]
Declination +37° 53′ 24.8854″[1]
Apparent magnitude (V) 4.95[2]
Characteristics
Evolutionary stage main sequence[3]
Spectral type A1 V[4]
U−B color index +0.01[2]
B−V color index +0.05[2]
R−I color index 0.03
Astrometry
Radial velocity (Rv)+5[5] km/s
Proper motion (μ) RA: +44.531[1] mas/yr
Dec.: −97.943[1] mas/yr
Parallax (π)20.1236 ± 0.2385 mas[1]
Distance162 ± 2 ly
(49.7 ± 0.6 pc)
Absolute magnitude (MV)+1.34[6]
Details
Mass2.29±0.04[3] M☉
Radius2.0[7] R☉
Luminosity27[6] L☉
Surface gravity (log g)4.33[4] cgs
Temperature9,230[4] K
Metallicity [Fe/H]–0.12[4] dex
Rotational velocity (v sin i)107[8] km/s
Age317[9] Myr
Other designations
ω Aur, 4 Aur, BD+37°1005, HD 31647, HIP 23179, HR 1592, SAO 57548, WDS J04593+3753AB[10]
Database references
SIMBADdata

Omega Aurigae, Latinized from ω Aurigae, is the Bayer designation for a double star[11] in the northern constellation of Auriga. Its apparent magnitude is 4.95,[2] 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).[1] The system is a member of the Columba group of co-moving stars.[12]

This is an A-type main sequence star with a stellar classification of A1 V.[4] 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[3] times the mass of the Sun and double[7] the Sun's radius. It is radiating 27[6] times the Sun's luminosity from its photosphere at an effective temperature of 9,230 K.[4] 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.[7] It has a magnitude 8.18 companion at an angular separation of 4.99 arcseconds.[11] The system is an X-ray source with a luminosity of 16.57×1029 ergs s−1.[13]

References

  1. ^ a b c d e f Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics. 616. A1. arXiv:1804.09365. Bibcode:2018A&A...616A...1G. doi:10.1051/0004-6361/201833051. Gaia DR2 record for this source at VizieR.
  2. ^ a b c d 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.
  3. ^ a b c 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.
  4. ^ a b c d e f 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.
  5. ^ Wilson, Ralph Elmer (1953), "General Catalogue of Stellar Radial Velocities", Carnegie Institute Washington D.C. Publication, Washington: Carnegie Institution of Washington, Bibcode:1953GCRV..C......0W.
  6. ^ a b c 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.
  7. ^ a b c 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. ^ a b Royer, F.; Zorec, J.; Gómez, A. E. (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. ^ a b 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. ^ "* ome Aur". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2012-08-24.
  11. ^ a b 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.
  12. ^ 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.
  13. ^ 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.

External links

This page was last edited on 29 November 2023, at 03:46
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