V538 Aurigae

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V538 Aurigae
Observation data
Epoch J2000      Equinox J2000
Constellation Auriga
Right ascension  05h 41m 20.33480s[1]
Declination +53° 28′ 51.8045″[1]
Apparent magnitude (V) 6.25[2]
Spectral type K1 V[3]
U−B color index 0.50[2]
B−V color index 0.84[2]
Variable type BY Dra[4]
Radial velocity (Rv)0.9[5] km/s
Proper motion (μ) RA: 1.82[1] mas/yr
Dec.: -523.99[1] mas/yr
Parallax (π)81.45 ± 0.54[1] mas
Distance40.0 ± 0.3 ly
(12.28 ± 0.08 pc)
Absolute magnitude (MV)5.75[6]
Mass0.871[5] M
Surface gravity (log g)4.55[5] cgs
Temperature5,257[5] K
Metallicity [Fe/H]+0.16[7] dex
Rotation11 days[7]
Rotational velocity (v sin i)2.80[4] km/s
Age3.76[5] Gyr
Other designations
BD+53° 934, GJ 211, HD 37394, HIP 26779, HR 1925, NSV 16618.[8]
Database references

V538 Aurigae is a star in the northern constellation of Auriga. With an apparent visual magnitude of 6.23, this star requires good dark sky conditions to view with the naked eye. It is located at a distance of 40.0 light-years (12.3 pc) from Earth.

This is a BY Draconis variable,[4] which means it undergoes changes in luminosity because regions of pronounced surface magnetic activity are moved into and out of the line of sight from the Earth as the star rotates (once every 11 days);[7] this has a spectral class of K1 V, indicating that it is a K-type main sequence star. It is a member of the Local Association,[3] and is most likely a thin disk star.[5]


  1. ^ a b c d e van Leeuwen, F. (2007), "Validation of the new Hipparcos reduction", Astronomy and Astrophysics, 474 (2): 653–664, arXiv:0708.1752, Bibcode:2007A&A...474..653V, doi:10.1051/0004-6361:20078357.
  2. ^ a b c Mermilliod, J.-C. (1986), "Compilation of Eggen's UBV data, transformed to UBV (unpublished)", Catalogue of Eggen's UBV data. SIMBAD, Bibcode:1986EgUBV........0M.
  3. ^ a b Montes, D.; et al. (November 2001), "Late-type members of young stellar kinematic groups - I. Single stars" (PDF), Monthly Notices of the Royal Astronomical Society, 328 (1): 45–63, arXiv:astro-ph/0106537, Bibcode:2001MNRAS.328...45M, doi:10.1046/j.1365-8711.2001.04781.x.
  4. ^ a b c Mishenina, T. V.; et al. (November 2012), "Activity and the Li abundances in the FGK dwarfs", Astronomy & Astrophysics, 547: 8, arXiv:1210.6843, Bibcode:2012A&A...547A.106M, doi:10.1051/0004-6361/201118412, A106
  5. ^ a b c d e f Ramírez, I.; et al. (February 2013), "Oxygen abundances in nearby FGK stars and the galactic chemical evolution of the local disk and halo", The Astrophysical Journal, 764 (1): 78, arXiv:1301.1582, Bibcode:2013ApJ...764...78R, doi:10.1088/0004-637X/764/1/78.
  6. ^ Holmberg, J.; et al. (July 2009), "The Geneva-Copenhagen survey of the solar neighbourhood. III. Improved distances, ages, and kinematics", Astronomy and Astrophysics, 501 (3): 941–947, arXiv:0811.3982, Bibcode:2009A&A...501..941H, doi:10.1051/0004-6361/200811191.
  7. ^ a b c Maldonado, J.; et al. (October 2010), "A spectroscopy study of nearby late-type stars, possible members of stellar kinematic groups", Astronomy and Astrophysics, 521: A12, arXiv:1007.1132, Bibcode:2010A&A...521A..12M, doi:10.1051/0004-6361/201014948.
  8. ^ "HR 1925 -- Variable of BY Dra type", SIMBAD Astronomical Database, Centre de Données astronomiques de Strasbourg, retrieved 2016-01-17.

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