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PU Aurigae

From Wikipedia, the free encyclopedia
Star in the constellation Auriga
PU Aurigae

Alight curve for PU Aurigae, plotted fromHipparcos data[1]
Observation data
Epoch J2000      Equinox J2000
ConstellationAuriga
Right ascension05h 18m 15.69826s[2]
Declination+42° 47′ 31.6133″[2]
Apparent magnitude (V)5.55[3]
Characteristics
Spectral typeM4 III[3]
B−Vcolor index1.492±0.012[3]
Variable typeLb[4]
Astrometry
Radial velocity (Rv)−38.41±1.02[3] km/s
Proper motion (μ)RA: +17.98[5]mas/yr
Dec.: −30.61[5]mas/yr
Parallax (π)5.7462±0.2309 mas[2]
Distance570 ± 20 ly
(174 ± 7 pc)
Absolute magnitude (MV)−0.63[3]
Details
Radius107[6] R☉
Luminosity1,523[6] L☉
Temperature3,482[6] K
Other designations
PU Aurigae,BD+42° 1239,HD 34269,HIP 24738,HR 1722,SAO 40214[7]
Database references
SIMBADdata

PU Aurigae is an irregular variable star located in the constellation Auriga. Ared giant, it varies by 0.1 magnitude around magnitude 5.64,[8] so it is faintly visible to thenaked eye. Located around 560 light-years distant, it shines with aluminosity approximately 1,523 times that of the Sun and has a surface temperature of 3,482 K.[6]

Although the star was first found to be variable byJoel Stebbins andCharles Morse Huffer in 1928,[9] it was not given itsvariable star designation until 1977.[10]

References

[edit]
  1. ^"Hipparcos Tools Interactive Data Access".Hipparcos. ESA. Retrieved8 December 2021.
  2. ^abcBrown, 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.
  3. ^abcdeAnderson, 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.
  4. ^Samus, N. N.; Durlevich, O. V.; et al. (2009). "VizieR Online Data Catalog: General Catalogue of Variable Stars (Samus+ 2007-2013)".VizieR On-line Data Catalog: B/GCVS. Originally Published in: 2009yCat....102025S.1.Bibcode:2009yCat....102025S.
  5. ^abvan Leeuwen, F. (November 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,S2CID 18759600.
  6. ^abcdMcDonald, I.; Zijlstra, A. A.; Boyer, M. L. (2012)."Fundamental Parameters and Infrared Excesses of Hipparcos Stars".Monthly Notices of the Royal Astronomical Society.427 (1):343–57.arXiv:1208.2037.Bibcode:2012MNRAS.427..343M.doi:10.1111/j.1365-2966.2012.21873.x.S2CID 118665352.
  7. ^"HD 34269".SIMBAD.Centre de données astronomiques de Strasbourg. Retrieved22 August 2018.
  8. ^Watson, Christopher (4 January 2010)."PU Aurigae".The International Variable Star Index.American Association of Variable Star Observers. Retrieved17 June 2015.
  9. ^Stebbins, Joel; Huffer, C. M. (1928)."The Constancy of the Light of Red Stars".Publications of the Washburn Observatory.15:137–174.Bibcode:1928PWasO..15..137S. Retrieved12 October 2024.
  10. ^Kukarkin, B. V.; Kholopov, P. N.; Fedorovich, V. P.; Kireyeva, N. N.; Kukarkina, N. P.; Medvedeva, G. I.; Perova, N. B. (March 1977)."62nd Name-List of Variable Stars"(PDF).Information Bulletin on Variable Stars.1248: 1.Bibcode:1977IBVS.1248....1K. Retrieved12 October 2024.
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