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64 Aurigae

From Wikipedia, the free encyclopedia

64 Aurigae
Observation data
Epoch J2000      Equinox J2000
Constellation Auriga
Right ascension 07h 18m 02.21420s[1]
Declination +40° 53′ 00.2248″[1]
Apparent magnitude (V) 5.87[2]
Characteristics
Evolutionary stage main sequence[3]
Spectral type A5 Vn[4]
B−V color index 0.181±0.005
Astrometry
Radial velocity (Rv)−10.0±4.3[2] km/s
Proper motion (μ) RA: −12.784[1] mas/yr
Dec.: +12.065[1] mas/yr
Parallax (π)10.4466 ± 0.1116 mas[1]
Distance312 ± 3 ly
(96 ± 1 pc)
Absolute magnitude (MV)1.22[2]
Details
Mass1.67[5] M☉
Luminosity27.03[2] L☉
Surface gravity (log g)3.88[5] cgs
Temperature8,014±272[5] K
Rotational velocity (v sin i)212[3] km/s
Age291[5] Myr
Other designations
64 Aur, BD+41°1630, FK5 276, HD 56221, HIP 35341, HR 2753, SAO 41679[6]
Database references
SIMBADdata

64 Aurigae is a single[7] star located 312[1] light years away from the Sun in the northern constellation of Auriga.[6] It is visible to the naked eye as a dim, white-hued star with an apparent magnitude of 5.87.[2] The star is moving closer to the Earth with a heliocentric radial velocity of −10, and may come to within 167 light-years in around 5.3 million years.[2] It is a member of the Sirius supercluster.[8]

This object is an ordinary A-type main-sequence star with a stellar classification of 5 Vn,[4] where the 'n' notation is used to indicate "nebulous" lines in the spectrum caused by rapid rotation. It is 291[5] million years old with a projected rotational velocity of 212 km/s.[3] The star has 1.67[5] times the mass of the Sun and is radiating 27[2] times the Sun's luminosity from its photosphere at an effective temperature of 8,014 K.[5]

It was also known to be part of a much bigger constellation named Telescopium Herschelii before it was unrecognized by the International Astronomical Union (IAU).

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 e f g 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.
  3. ^ a b c Zorec, J.; Royer, F.; Asplund, Martin; Cassisi, Santi; Ramirez, Ivan; Melendez, Jorge; Bensby, Thomas; Feltzing, Sofia (2012), "Rotational velocities of A-type stars. IV. Evolution of rotational velocities", Astronomy and Astrophysics, 537: A120, arXiv:1201.2052, Bibcode:2012A&A...537A.120Z, doi:10.1051/0004-6361/201117691, S2CID 55586789.
  4. ^ a b Cowley, A.; et al. (April 1969), "A study of the bright A stars. I. A catalogue of spectral classifications", Astronomical Journal, 74: 375–406, Bibcode:1969AJ.....74..375C, doi:10.1086/110819.
  5. ^ a b c d e f g 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.
  6. ^ a b "63 Aur". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2019-05-24.
  7. ^ 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.
  8. ^ Palous, J.; Hauck, B. (July 1986), "The Sirius supercluster", Astronomy and Astrophysics, 162: 54–61, Bibcode:1986A&A...162...54P.
This page was last edited on 2 November 2023, at 09:08
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