V602 Carinae

V602 Carinae (V602 Car, HD 97671) is a red supergiant and variable star of spectral type of M3 in the constellation Carina. It is one of largest known stars.

V602 Carinae

Location of V602 Car
Observation data
Epoch J2000.0      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
Spectral type M3 Ia-Iab[4]
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[5] mas/yr
Dec.: 2.183[5] mas/yr
Parallax (π)0.4366 ± 0.0698[5] mas
Distance1,977±75[6] pc
Absolute magnitude (MV)−5.85 (variable)[7]
Details
Mass17.7[8] M☉
Radius932[9] R☉
Luminosity125,000 - 131,000[9] L☉
Surface gravity (log g)−0.3±0.16[6] cgs
Temperature3,550±170[9] K
Other designations
V602 Carinae, V602 Car, HD 97671, CD−59°3623, IRAS 11113-5949, 2MASS J11132996-6005288
Database references
SIMBADdata

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.[7] 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.[6] More recent measurements based on a Gaia Data Release 2 parallax of 0.4366±0.0698 mas gives a luminosity below 125,000–131,000 L☉ with a corresponding radius of 932 R☉ based on the same effective temperature derived in 2005.[9]

V602 Car has an estimated mass loss rate of 1.9×10−6 M☉ per year.[2] 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.[10]

V602 Car is a semiregular variable star with a maximum brightness range of magnitude 7.6 - 9.1[11] and a period of 635[11] or 672[3] days. Despite the large amplitude of variation, it was only named as a variable star in 2006.[3][11]

See also

References
  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. Mauron, N.; Josselin, E. (February 2011), "The mass-loss rates of red supergiants and the de Jager prescription", Astronomy and Astrophysics, 526: A156, arXiv:1010.5369, Bibcode:2011A&A...526A.156M, doi:10.1051/0004-6361/201013993.
  3. 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.
  4. Keenan, Philip C.; McNeil, Raymond C. (1989). "The Perkins catalog of revised MK types for the cooler stars". Astrophysical Journal Supplement Series. 71: 245. Bibcode:1989ApJS...71..245K. doi:10.1086/191373.
  5. 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.
  6. Arroyo-Torres, B.; Wittkowski, M.; Chiavassa, A.; Scholz, M.; Freytag, B.; Marcaide, J. M.; Hauschildt, P. H.; Wood, P. R.; Abellan, F. J. (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. arXiv:1501.01560. Bibcode:2015A&A...575A..50A. doi:10.1051/0004-6361/201425212.
  7. 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. arXiv:astro-ph/0504337. Bibcode:2005ApJ...628..973L. doi:10.1086/430901.
  8. Fadeyev, Yu. A. (2012). "Nonlinear pulsations of red supergiants". Astronomy Letters. 38 (4): 260–270. arXiv:1112.2365. Bibcode:2012AstL...38..260F. doi:10.1134/S1063773712040032.
  9. 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. arXiv:1905.03744. Bibcode:2019AJ....158...20M. doi:10.3847/1538-3881/ab1cbd.
  10. Humphreys, Roberta M.; Strecker, Donald W.; Ney, E. P. (February 1972), "Spectroscopic and Photometric Observations of M Supergiants in Carina", Astrophysical Journal, 172: 75, Bibcode:1972ApJ...172...75H, doi:10.1086/151329.
  11. 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.
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