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VY Canis Majoris
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VY Canis Majoris
Actual image of VY Canis Majoris (brightest star in the image) and its surrounding molecular cloud complex in the open cluster NGC 2362 as seen from the Rutherfurd Observatory of the Columbia University in New York, United States on the evening of 7 September 2014, Sunday.
Observation data
Epoch J2000 Equinox J2000
Constellation
Canis Major
Right ascension
07h 22m 58.32877s
Declination
-25° 46' 03.2355?
Apparent magnitude (V)
6.5 to 9.6
7.9607
Characteristics
Spectral type
(M2.5I-)M3-M4.5
Variable type
Semiregular
Astrometry
Radial velocity (Rv)
41 km/s
Proper motion (µ)
RA: 9.84 mas/yr
Dec.: 0.75 mas/yr
Parallax (p)
0.83 ± 0.1 mas
Distance
~3,840 ly
(1,170 pc)
Details
Mass
17 ± 8 M?
Radius
1420 ± 120 R?
Luminosity
~270,000 L?
Surface gravity (log g)
-0.6 cgs
Temperature
~3,490 K
Other designations
Database references
SIMBAD
data
VY Canis Majoris (VY CMa) is a red hypergiant star located in the constellation Canis Major. It is one of the largest stars (at one time it was the largest known) and also one of the most luminous of its type, and has a radius of approximately 1,420 ± 120 solar radii (equal to a diameter of 13.2 astronomical units, or about 1,976,640,000 km), and is located about 1.2 kiloparsecs (3,900 light-years) from Earth.VY Canis Majoris is a single star categorized as a semiregular variable with an estimated period of 2,000 days. It has an average density of 5 to 10 mg/m3. If placed at the center of the Solar System, VY Canis Majoris's surface would extend beyond the orbit of Jupiter, although there is still considerable variation in estimates of the radius.
^ a b c d e Van Leeuwen, F. (2007). "Validation of the new Hipparcos reduction". Astronomy and Astrophysics 474 (2): 653. arXiv:0708.1752. Bibcode:2007A&A...474..653V. doi:10.1051/0004-6361:20078357.
^ "GCVS Query=VY CMa". General Catalogue of Variable Stars @ Sternberg Astronomical Institute, Moscow, Russia. Retrieved 2010-11-24.
^ Cite error: The named reference Massey2006 was invoked but never defined (see the help page).
^ a b c d e f g Wittkowski, M.; Hauschildt, P.H.; Arroyo-Torres, B.; Marcaide, J.M. (5 April 2012). "Fundamental properties and atmospheric structure of the red supergiant VY CMa based on VLTI/AMBER spectro-interferometry". Astronomy & Astrophysics 540: L12. arXiv:1203.5194. Bibcode:2012A&A...540L..12W. doi:10.1051/0004-6361/201219126.
^ Monnier, J. D.; Geballe, T. R.; Danchi, W. C. (1 August 1998). "Temporal variations of midinfrared spectra in late-type stars". The Astrophysical Journal (American Astronomical Society) 502 (2): 833–846. arXiv:astro-ph/9803027. Bibcode:1998ApJ...502..833M. doi:10.1086/305945.
^ Humphreys, Roberta M.; Helton, L. Andrew; Jones, Terry J. (2007). "The Three-Dimensional Morphology of VY Canis Majoris. I. The Kinematics of the Ejecta". The Astronomical Journal 133 (6): 2716. arXiv:astro-ph/0702717. Bibcode:2007AJ....133.2716H. doi:10.1086/517609.
^ Zhang, B.; Reid, M. J.; Menten, K. M.; Zheng, X. W. (January 2012) . "Distance and Kinematics of the Red Hypergiant VY CMa: VLBA and VLA Astrometry". The Astrophysical Journal 744 (1): 23. arXiv:1109.3036. Bibcode:2012ApJ...744...23Z. doi:10.1088/0004-637X/744/1/23.
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