VY Canis Majoris
 Size comparison atween the Sun an VY Canis Majoris | |
| Observation data EpochJ2000EquinoxJ2000 | |
|---|---|
| Constellation | Canis Major |
| Richt ascension | 07h22m58.32877s[1] |
| Declination | −25° 46′ 03.2355″[1] |
| Apparent magnitude(V) | 6.5 to 9.6[2] 7.9607[3] |
| Chairactereestics | |
| Spectral type | M3[4]-M5e Ia[5] |
| B−Vcolour index | 2.24[4] |
| Variable teep | Semiregular[6] |
| Astrometry | |
| Radial velocity(Rv) | 49 ± 10[4]km/s |
| Proper motion(μ) | RA:9.84[4]mas/yr Dec.:0.75[4]mas/yr |
| Parallax(π) | 0.83 ± 0.1[7]mas |
| Distance | ~3,840ly (1,170[8] [9]pc) |
| Details | |
| Mass | 17 ± 8[8]M☉ |
| Radius | 1420 ± 120[8]R☉ |
| Luminosity | ~270,000[8]L☉ |
| Surface gravity(logg) | -0.6[8]cgs |
| Temperatur | ~3,490[8]K |
| Age | 8.2×106[10]years |
| Ither designations | |
VY Canis Majoris(VY CMa) is a reidhypergiantin the constellationCanis Major.It is ane o thelairgest kent starnsbi radius an an aaane o the maist luminouso itstype.It is approximately 1,420 ± 120solar radii[8](equal tae 6.6astronomical units,sicweys a diameter aboot 1,975,000,000 kilometres (1.227×109 mi)), an aboot 1.2kiloparsec(3,900 light-year) distant fraeYird.VY CMa is a singlestarncategorized as asemiregular variablean haes an estimatit period o 2,000 days. It haes an average density o 5 tae 10 mg/m3.If placed at the centre o theSolar Seestem,VY Canis Majoris's surface wad extend ayond the orbit oJupiter,altho thare is still considerable variation in estimates o the radius, wi some makin it lairger than the orbit oSaturn.[11]
References
[eedit|eedit soorce]- ↑ab"SIMBAD basic query result: VY Canis Majoris".SIMBAD, Centre de Données astronomiques de Strasbourg.Retrieved23 Januar2013.
- ↑"GCVS Query=VY CMa".General Catalogue of Variable Stars@Sternberg Astronomical Institute, Moscow, Russia.Retrieved24 November2010.
- ↑ab"Hipparchos catalogue: query form".CASU Astronomical Data Centre.Cambridge Astronomical Survey Unit. 2006. Archived fraethe originalon 3 Mairch 2016.Retrieved10 Mairch2009.
- ↑abcde"SIMBAD basic query result: VY Canis Majoris".SIMBAD, Centre de Données astronomiques de Strasbourg.Retrieved7 Mairch2009.
- ↑abLipscy, S. J.; Jura, M.; Reid, M. J. (10 Juin 2005)."Radio photosphere and mass-loss envelope of VY Canis Majoris".The Astrophysical Journal.The American Astronomical Society.626(1): 439–445.arXiv:astro-ph/0502586.Bibcode:2005ApJ...626..439L.doi:10.1086/429900.
- ↑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.
- ↑"Distance and Kinematics of the Red Hypergiant VY CM".Retrieved19 Mey2012.
- ↑abcdefgWittkowski, M.; Hauschildt, P.H.; Arroyo-Torres, B.; Marcaide, J.M. (5 Apryle 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.
- ↑ Y. K. Choi; Hirota, Tomoya; Honma, Mareki; Kobayashi, Hideyuki; Bushimata, Takeshi; Imai, Hiroshi; Iwadate, Kenzaburo; Jike, Takaaki; Kameno, Seiji (2008). "Distance to VY VMa with VERA".Publications of the Astronomical Society of Japan.Publications Astronomical Society of Japan.60:1007.arXiv:0808.0641.Bibcode:2008PASJ...60.1007C.
- ↑Zhang, B.; Reid, M. J.; Menten, K. M.; Zheng, X. W. (December 2011)."DISTANCE AND KINEMATICS OF THE RED HYPERGIANT VY CMa: VERY LONG BASELINE ARRAY AND VERY LARGE ARRAY ASTROMETRY".The Astrophysical Journal(in Inglis).744(1): 23.doi:10.1088/0004-637X/744/1/23.ISSN0004-637X.
- ↑Massey, Philip; Levesque, Emily M.; Plez, Bertrand (1 August 2006)."Bringing VY Canis Majoris down to size: an improved determination of its effective temperature".The Astrophysical Journal.646(2): 1203–1208.arXiv:astro-ph/0604253.Bibcode:2006ApJ...646.1203M.doi:10.1086/505025.