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V602 Carinae

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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 mas[5]
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

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.

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. ^ a b 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. ^ a b c d 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. ^ a b c d 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. ^ a b c 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. ^ a b c 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. ^ a b 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. ^ a b c d 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.{{cite journal}}: CS1 maint: unflagged free DOI (link)
  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. ^ a b c 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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