Astronomy:Omega Aurigae

From HandWiki
Short description: Star in the constellation Auriga
"HR 1592" redirects here. For the legislation, see Matthew Shepard Act.
Omega Aurigae
Location of ω Aurigae (circled in red)
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
Distance162 ± 2 ly
(49.7 ± 0.6 pc)
Absolute magnitude (MV)+1.34[1]
Details
ω Aur A
Mass2.29±0.04[4] M☉
Radius2.0[7] R☉
Luminosity27[1] L☉
Surface gravity (log g)4.33[5] cgs
Temperature9,230[5] K
Metallicity [Fe/H]−0.12[5] dex
Rotational velocity (v sin i)107[8] km/s
Age317[9] Myr
ω Aur B
Mass1.1[10] 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[11]
Database references
SIMBADdata

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. ↑ 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. ↑ 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. ↑ 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. ↑ 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. ↑ 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. ↑ 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. ↑ 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. ↑ 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. ↑ 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. ↑ 10.0 10.1 Gratton, R. et al. (May 2024), "Stellar companions and Jupiter-like planets in young associations", Astronomy & Astrophysics 685: id. A119, doi:10.1051/0004-6361/202348393, Bibcode: 2024A&A...685A.119G. 
  11. ↑ "* ome Aur". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=%2A+ome+Aur. 
  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, doi:10.1111/j.1365-2966.2008.13596.x, Bibcode: 2008MNRAS.389..869E. 
  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, doi:10.1051/0004-6361/201628253, A13, Bibcode: 2016A&A...590A..13E. 
  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, doi:10.1086/378164, Bibcode: 2003AJ....126.1996M. 



Retrieved from "https://handwiki.org/wiki/index.php?title=Astronomy:Omega_Aurigae&oldid=4391915"