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65 Aurigae

From Wikipedia, the free encyclopedia
Binary star system in the constellation Auriga
65 Aurigae
Observation data
Epoch J2000      Equinox J2000
ConstellationAuriga
Right ascension07h 22m 02.61744s[1]
Declination+36° 45′ 38.0957″[1]
Apparent magnitude (V)5.12[2]
Characteristics
Spectral typeK0 III[3]
B−Vcolor index1.082±0.005[2]
Astrometry
Radial velocity (Rv)21.81±0.16[2] km/s
Proper motion (μ)RA: −96.915[1]mas/yr
Dec.: −22.436[1]mas/yr
Parallax (π)12.9673±0.1294 mas[1]
Distance252 ± 3 ly
(77.1 ± 0.8 pc)
Absolute magnitude (MV)0.82[2]
Details
65 Aur A
Mass1.34[4] M
Radius13.02+0.47
−2.57
[1] R
Luminosity69.6±0.9[1] L
Surface gravity (log g)2.72[3] cgs
Temperature4,575±17[4] K
Metallicity [Fe/H]−0.35±0.04[2] dex
Rotational velocity (v sin i)0.0[5] km/s
Age3.31[4] Gyr
Other designations
65 Aur,BD+37°1707,FK5 2568,HD 57264,HIP 35710,HR 2793,SAO 60010[6]
Database references
SIMBADdata

65 Aurigae is abinary star[7] system located 252 light years away from the Sun in the northernconstellation ofAuriga. It is visible to the naked eye as a faint, orange hued star with anapparent visual magnitude of 5.12.[2] The primary, designated component A, is an aginggiant star with astellar classification of K0 III.[3] It is 3.31[4] billion years old and has expanded to 13 times theSun's radius after exhausting the hydrogen at itscore.[1] Its companion, component B, is a magnitude 11.7 star located at anangular separation of11.4 from the primary, as of 2008.[7] The pair are moving further from the Earth with a heliocentricradial velocity of 22 km/s.[2]

It was also known to be part of a much bigger constellation namedTelescopium Herschelii before it was unrecognized by theInternational Astronomical Union (IAU).

References

[edit]
  1. ^abcdefghBrown, 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 atVizieR.
  2. ^abcdefgAnderson, 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. ^abcCenarro, A. J.; et al. (January 2007), "Medium-resolution Isaac Newton Telescope library of empirical spectra - II. The stellar atmospheric parameters",Monthly Notices of the Royal Astronomical Society,374 (2):664–690,arXiv:astro-ph/0611618,Bibcode:2007MNRAS.374..664C,doi:10.1111/j.1365-2966.2006.11196.x,S2CID 119428437.
  4. ^abcdLuck, R. Earle (2015), "Abundances in the Local Region. I. G and K Giants",The Astronomical Journal,150 (3): 88,arXiv:1507.01466,Bibcode:2015AJ....150...88L,doi:10.1088/0004-6256/150/3/88,S2CID 118505114.
  5. ^Massarotti, Alessandro; et al. (January 2008), "Rotational and Radial Velocities for a Sample of 761 Hipparcos Giants and the Role of Binarity",The Astronomical Journal,135 (1):209–231,Bibcode:2008AJ....135..209M,doi:10.1088/0004-6256/135/1/209,S2CID 121883397.
  6. ^"65 Aur".SIMBAD.Centre de données astronomiques de Strasbourg. Retrieved2019-05-25.
  7. ^abEggleton, 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.

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