Astronomy:V602 Carinae

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Short description: Star in the constellation Carina
V602 Carinae
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Location of V602 Car
Observation data
Equinox J2000.0]] (ICRS)
Constellation Carina
Right ascension  11h 13m 29.9740s[1]
Declination −60° 05′ 28.838″[1]
Apparent magnitude (V) 8.39[2] (7.6 - 9.1[3])
Characteristics
Evolutionary stage Red supergiant[4] or hypergiant[5][6][7]
Spectral type M3 Ia-Iab[8]
U−B color index +2.59[2]
B−V color index +2.52[2]
Variable type SRc[3]
Astrometry
Proper motion (μ) RA: −5.425[9] mas/yr
Dec.: +2.183[9] mas/yr
Parallax (π)0.4366 ± 0.0698[9] mas
Distanceapprox. 7,000 ly
(approx. 2,300 pc)
Absolute magnitude (MV)−4.83 (variable)[10]
Details
Mass17.7[11] – 20[12] M☉
Radius1,015[12] R☉
Luminosity126,000[12] L☉
Surface gravity (log g)−0.5[12] cgs
Temperature3,400[12] K
Other designations
V602 Carinae, V602 Car, HD 97671, CD−59°3623, IRAS 11113−5949, 2MASS J11132996−6005288
Database references
SIMBADdata

V602 Carinae (V602 Car, HD 97671) is a red supergiant or hypergiant[5][6][7] variable star of spectral type M3 in the constellation Carina. It is considered to be one of largest known stars, being around 1,000 times larger than the Sun.[12]

Variability

A visual band light curve for V602 Carinae, plotted from AAVSO data

V602 Car is a semiregular variable star with a maximum brightness range of magnitude 7.6 - 9.1[13] and a period of 635[13] or 672[3] days. Despite the large amplitude of variation, it was only named as a variable star in 2006.[3][13]

Properties

V602 Carinae is a red supergiant with a spectral type given in the General Catalogue of Variable Stars as M3Ia+,[3] suggesting the star is a hypergiant or an extremely luminous supergiant. It has been defined as a standard star for the MK spectral classification of M3Ia-Iab, which suggests the star is an intermediate-luminosity supergiant.[8]

In 2005, V602 Car was calculated to have a bolometric luminosity below 110,000 L☉ and a radius around 860 R☉ based on the assumption of an effective temperature of 3,550 K.[4] A 2015 study derived a slightly higher bolometric luminosity of 138,000+66,000
−45,000 L☉ based on the measured flux and an assumed distance, and a larger radius of 1,050±165 R☉ based on the measured angular diameter and luminosity. An effective temperature of 3,432±280 K was then calculated from the luminosity and radius.[14] A more recent measurement based on a Gaia Data Release 2 parallax of 0.4366±0.0698 mas gives a luminosity at 125,000–131,000 L☉ with a corresponding radius of 932 R☉ based on the same effective temperature derived in 2005.[15] The radius was measured again in 2024 at 1,015 R☉.[12]

V602 Car has an estimated mass loss rate of 1×10−5 M☉ per year.[12] An excess of emission at long wavelengths from this star, as well as a small amount of silicate emission, suggests that it may be enclosed by an extensive cloud of dust.[16]

See also

References

  1. ↑ 1.0 1.1 Hog, E.; Kuzmin, A.; Bastian, U.; Fabricius, C.; Kuimov, K.; Lindegren, L.; Makarov, V. V.; Roeser, S. (1998). "The TYCHO Reference Catalogue". Astronomy and Astrophysics 335: L65. Bibcode: 1998A&A...335L..65H. 
  2. ↑ 2.0 2.1 2.2 Mauron, N.; Josselin, E. (February 2011), "The mass-loss rates of red supergiants and the de Jager prescription", Astronomy and Astrophysics 526: A156, doi:10.1051/0004-6361/201013993, Bibcode: 2011A&A...526A.156M. 
  3. ↑ 3.0 3.1 3.2 3.3 3.4 Samus, N. N. 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. 
  4. ↑ 4.0 4.1 Levesque, Emily M.; Massey, Philip; Olsen, K. A. G.; Plez, Bertrand; Josselin, Eric; Maeder, Andre; Meynet, Georges (2005). "The Effective Temperature Scale of Galactic Red Supergiants: Cool, but Not as Cool as We Thought". The Astrophysical Journal 628 (2): 973–985. doi:10.1086/430901. Bibcode: 2005ApJ...628..973L. 
  5. ↑ 5.0 5.1 Samus', N. N.; Kazarovets, E. V.; Durlevich, O. V.; Kireeva, N. N.; Pastukhova, E. N. (2017). "General catalogue of variable stars: Version GCVS 5.1". Astronomy Reports 61 (1): 80. doi:10.1134/S1063772917010085. Bibcode: 2017ARep...61...80S. 
  6. ↑ 6.0 6.1 Skiff, B. A. (2014). "VizieR Online Data Catalog: Catalogue of Stellar Spectral Classifications (Skiff, 2009-2016)". VizieR On-line Data Catalog: B/Mk. Originally Published in: Lowell Observatory (October 2014) 1: B/mk. Bibcode: 2014yCat....1.2023S. 
  7. ↑ 7.0 7.1 Jones, Terry (2025). "Red and Yellow Hypergiants". Galaxies 13 (2): 43. doi:10.3390/galaxies13020043. Bibcode: 2025Galax..13...43J. 
  8. ↑ 8.0 8.1 Keenan, Philip C.; McNeil, Raymond C. (1989). "The Perkins catalog of revised MK types for the cooler stars". Astrophysical Journal Supplement Series 71: 245. doi:10.1086/191373. Bibcode: 1989ApJS...71..245K. 
  9. ↑ 9.0 9.1 9.2 Brown, A. G. A. (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics 616: A1. doi:10.1051/0004-6361/201833051. Bibcode: 2018A&A...616A...1G.  Gaia DR2 record for this source at VizieR.
  10. ↑ Melnik, A. M.; Dambis, A. K. (2020). "Distance scale for high-luminosity stars in OB associations and in field with Gaia DR2. Spurious systematic motions". Astrophysics and Space Science 365 (7): 112. doi:10.1007/s10509-020-03827-0. Bibcode: 2020Ap&SS.365..112M. 
  11. ↑ Fadeyev, Yu. A. (2012). "Nonlinear pulsations of red supergiants". Astronomy Letters 38 (4): 260–270. doi:10.1134/S1063773712040032. Bibcode: 2012AstL...38..260F. 
  12. ↑ 12.0 12.1 12.2 12.3 12.4 12.5 12.6 12.7 González-Torà, G.; Wittkowski, M.; Davies, B.; Plez, B. (December 19, 2023). "The effect of winds on atmospheric layers of red supergiants II. Modelling VLTI/GRAVITY and MATISSE observations of AH Sco, KW Sgr, V602 Car, CK Car and V460 Car". Astronomy & Astrophysics 683: A19. doi:10.1051/0004-6361/202348047. ISSN 0004-6361. 
  13. ↑ 13.0 13.1 13.2 Kazarovets, E. V.; Samus, N. N.; Durlevich, O. V.; Kireeva, N. N.; Pastukhova, E. N. (2006). "The 78th Name-List of Variable Stars". Information Bulletin on Variable Stars 5721: 1. Bibcode: 2006IBVS.5721....1K. 
  14. ↑ Arroyo-Torres, B.; Wittkowski, M.; Chiavassa, A.; Scholz, M.; Freytag, B.; Marcaide, J. M.; Hauschildt, P. H.; Wood, P. R. et al. (2015). "What causes the large extensions of red supergiant atmospheres?. Comparisons of interferometric observations with 1D hydrostatic, 3D convection, and 1D pulsating model atmospheres". Astronomy & Astrophysics 575: A50. doi:10.1051/0004-6361/201425212. Bibcode: 2015A&A...575A..50A. 
  15. ↑ Messineo, M.; Brown, A. G. A. (2019). "A Catalog of Known Galactic K-M Stars of Class I Candidate Red Supergiants in Gaia DR2". The Astronomical Journal 158 (1): 20. doi:10.3847/1538-3881/ab1cbd. Bibcode: 2019AJ....158...20M. 
  16. ↑ Humphreys, Roberta M.; Strecker, Donald W.; Ney, E. P. (February 1972), "Spectroscopic and Photometric Observations of M Supergiants in Carina", Astrophysical Journal 172: 75, doi:10.1086/151329, Bibcode: 1972ApJ...172...75H. 



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