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V520 Carinae

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V520 Carinae

A light curve for V520 Carinae, plotted from Hipparcos data[1]
Observation data
Epoch J2000      Equinox J2000
Constellation Carina
Right ascension 10h 43m 32.29015s[2]
Declination −60° 33′ 59.8308″[2]
Apparent magnitude (V) +4.58[3] (4.50 to 4.59)
Characteristics
Spectral type K4III[4]
B−V color index +1.700±0.059[3]
Variable type Lc:[5]
Astrometry
Radial velocity (Rv)+9.1±0.3[3] km/s
Proper motion (μ) RA: −14.75[2] mas/yr
Dec.: +3.10[2] mas/yr
Parallax (π)2.86 ± 0.17 mas[2]
Distance1,140 ± 70 ly
(350 ± 20 pc)
Absolute magnitude (MV)−3.63[3]
Details
Mass7.9±0.1[6] M☉
Radius131.18+4.67
−6.61[7] R☉
Luminosity3,599±297[7] L☉
Temperature3,903+102
−68[7] K
Age33.3±5.1[6] Myr
Other designations
w Car, V520 Car, NSV 4951, CD−59°3262, FK5 2524, GC 14762, HD 93070, HIP 52468, HR 4200, SAO 251090[8]
Database references
SIMBADdata

V520 Carinae is a single[9] star in the southern constellation of Carina. It has the Bayer designation w Carinae, while V520 Carinae is a variable star designation. The star has an orange hue and is faintly visible to the naked eye with an apparent visual magnitude that fluctuates around +4.58.[3] It is located at a distance of approximately 1,140 light years from the Sun based on parallax, and it is drifting further away with a radial velocity of +9 km/s.[3] It is a candidate member of the IC 2391 moving group of co-moving stars.[10]

This is an aging giant star with a stellar classification of K4III,[4] although Humphreys (1970) found a supergiant class of K3Ib.[11] It is a suspected slow irregular variable of type Lc and its brightness varies from magnitude +4.50 to +4.59 with no periodicity.[12] The star now has 131 times the girth of the Sun,[7] having exhausted the supply of hydrogen at its core then cooled and expanded. Comparison with theoretical evolutionary tracks suggests it is 33 million years old with 7.9 times the mass of the Sun,[6] although analysis of its motion suggests it may be an astrometric binary with a mass of 1.014 M☉.[13] The star is radiating 3,600[7] times the luminosity of the Sun from its enlarged photosphere at an effective temperature of 3,903 K.[7]

References

  1. ^ "Hipparcos Tools Interactive Data Access". Hipparcos. ESA. Retrieved 8 December 2021.
  2. ^ 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, S2CID 18759600.
  3. ^ a b c d e f 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.
  4. ^ a b Houk, Nancy; Cowley, A. P. (1979), Michigan catalogue of two-dimensional spectral types for the HD stars, vol. 1, Ann Arbor, Michigan: Dept. of Astronomy, University of Michigan, Bibcode:1978mcts.book.....H.
  5. ^ Samus, N. N.; et al. (2017), "General Catalogue of Variable Stars", Astronomy Reports, 5.1, 61 (1): 80–88, Bibcode:2017ARep...61...80S, doi:10.1134/S1063772917010085, S2CID 125853869.
  6. ^ a b c Tetzlaff, N.; et al. (January 2011), "A catalogue of young runaway Hipparcos stars within 3 kpc from the Sun", Monthly Notices of the Royal Astronomical Society, 410 (1): 190–200, arXiv:1007.4883, Bibcode:2011MNRAS.410..190T, doi:10.1111/j.1365-2966.2010.17434.x, S2CID 118629873.{{citation}}: CS1 maint: unflagged free DOI (link)
  7. ^ 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.
  8. ^ "V520 Car". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2020-02-19.
  9. ^ 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.{{citation}}: CS1 maint: unflagged free DOI (link)
  10. ^ Montes, D.; et al. (November 2001), "Late-type members of young stellar kinematic groups - I. Single stars", 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, S2CID 55727428.{{citation}}: CS1 maint: unflagged free DOI (link)
  11. ^ Humphreys, R. M. (June 1970), "The space distribution and kinematics of supergiants", Astronomical Journal, 75: 602–623, Bibcode:1970AJ.....75..602H, doi:10.1086/110995
  12. ^ "V520 Carinae", Variable Star Index, retrieved 2020-02-20
  13. ^ Kervella, Pierre; Arenou, Frédéric; Mignard, François; Thévenin, Frédéric (2019), "Stellar and substellar companions of nearby stars from Gaia DR2. Binarity from proper motion anomaly", Astronomy and Astrophysics, 623: A72, arXiv:1811.08902, Bibcode:2019A&A...623A..72K, doi:10.1051/0004-6361/201834371, S2CID 119491061.
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