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] |
| Distance | 312 ± 3 ly (96 ± 1 pc) |
| Absolute magnitude (MV) | 1.22[2] |
| Details | |
| Mass | 1.67[5] M☉ |
| Luminosity | 27.03[2] L☉ |
| Surface gravity (log g) | 3.88[5] cgs |
| Temperature | 8,014±272[5] K |
| Rotational velocity (v sin i) | 212[3] km/s |
| Age | 291[5] Myr |
| Other designations | |
| Database references | |
| SIMBAD | data |
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
[edit]- ^ 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.
- ^ 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.
- ^ 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.
- ^ 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.
- ^ 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.
- ^ a b "63 Aur". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2019-05-24.
- ^ 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.
- ^ Palous, J.; Hauck, B. (July 1986), "The Sirius supercluster", Astronomy and Astrophysics, 162: 54–61, Bibcode:1986A&A...162...54P.
