Movatterモバイル変換

[0]ホーム
URL:

Jump to content
WikipediaThe Free Encyclopedia
Search

Omega Canis Majoris

From Wikipedia, the free encyclopedia
Star in the constellation Canis Major
ω Canis Majoris
Location of ω Canis Majoris (circled)
Observation data
EpochJ2000.0      EquinoxJ2000.0 (ICRS)
ConstellationCanis Major[1]
Right ascension07h 14m 48.654s[2]
Declination−26° 46′ 21.60″[2]
Apparent magnitude (V)3.60 to 4.18[3]
Characteristics
Spectral typeB2.5Ve[4]
U−Bcolor index−0.73[5]
B−Vcolor index−0.14[5]
Variable typeγ Cas[3]
Astrometry
Radial velocity (Rv)23.2±2.4[6] km/s
Proper motion (μ)RA: −11.617mas/yr[2]
Dec.: +8.109mas/yr[2]
Parallax (π)3.5610±0.1524 mas[2]
Distance920 ± 40 ly
(280 ± 10 pc)
Absolute magnitude (MV)−3.21[1]
Details
Mass10.1±0.7[7] M☉
Radius6.2[8] R☉
Luminosity13,081[9] L☉
Surface gravity (log g)3.5[10] cgs
Temperature21,878[10] K
Rotational velocity (v sin i)80[11] km/s
Age22.5±2.6[7] Myr
Other designations
ω CMa,28 Canis Majoris,CD−26°4073,GC 9625,HD 56139,HIP 35037,HR 2749,SAO 173282[12]
Database references
SIMBADdata

Omega Canis Majoris is a solitary,[13] blue-white-huedstar in the equatorialconstellation ofCanis Major. Its name is aBayer designation that isLatinized from ω Canis Majoris, and abbreviated Omega CMa or ω CMa. This star is visible to thenaked eye with anapparent visual magnitude of about 4. Based upon an annualparallax shift of3.56 mas as seen fromEarth,[2] this system is located roughly 920light-years (280 pc) away from theSun. It is drifting further away with a line of sight velocity of 23 km/s.[6]

Properties

[edit]
Avisual bandlight curve for Omega Canis Majoris, adapted from Šteflet al. (2003)[14]

This star has astellar classification of B2.5Ve, indicating it is amain sequenceBe star, although it has also been classified as asubgiant.[15] One of the most observed Be stars of theSouthern Hemisphere,[16] Omega Canis Majoris is classified as aGamma Cassiopeiae-typevariable star.[3] Both theluminosity and theradial velocity vary with a primary cyclical period of 1.372 days.[17] The variation in brightness, ranging from magnitude +3.60 to +4.18,[3] shows changes over time, which suggests there are two overlapping periods of 1.37 and 1.49 days. The star also undergoes transient periodicities following outbursts.[18][11]

This is amassive star with ten[7] times themass of the Sun and 6.2[8] times theSun's radius. At an estimated age of 22.5 million years,[7] it is radiating 13,081[9] times theSun's luminosity from itsphotosphere at aneffective temperature of 21,878 K.[10] The star is being viewed nearly pole on, so the measuredprojected rotational velocity of 80 km/s is only a fraction of the true equatorial velocity, estimated as 350 km/s. It is surrounded by a symmetric circumstellardecretion disk of material that is being heated by the star, which in turn is insertingemission lines into the combined spectrum.[11]

References

[edit]
  1. ^abAnderson, E.; Francis, Ch. (2012), "XHIP: An extended hipparcos compilation",Astronomy Letters,38 (5): 331,arXiv:1108.4971,Bibcode:2012AstL...38..331A,doi:10.1134/S1063773712050015. XHIP record for this object atVizieR.
  2. ^abcdeVallenari, A.; et al. (Gaia collaboration) (2023),"Gaia Data Release 3. Summary of the content and survey properties",Astronomy and Astrophysics,674: A1,arXiv:2208.00211,Bibcode:2023A&A...674A...1G,doi:10.1051/0004-6361/202243940,S2CID 244398875. Gaia DR3 record for this source atVizieR.
  3. ^abcdSamus, N. N.; et al. (2017), "General Catalogue of Variable Stars",Astronomy Reports, 5.1,61 (1):80–88,Bibcode:2017ARep...61...80S,doi:10.1134/S1063772917010085,S2CID 125853869.
  4. ^Slettebak, A. (1982), "Spectral types and rotational velocities of the brighter Be stars and A-F type shell stars",Astrophysical Journal Supplement Series,50:55–83,Bibcode:1982ApJS...50...55S,doi:10.1086/190820, 80.
  5. ^abFeinstein, A.; Marraco, H. G. (November 1979), "The photometric behavior of Be Stars",Astronomical Journal,84:1713–1725,Bibcode:1979AJ.....84.1713F,doi:10.1086/112600.
  6. ^abGontcharov, G. A. (2006), "Pulkovo compilation of radial velocities for 35495 stars in a common system",Astronomy Letters,32 (11):759–771,arXiv:1606.08053,Bibcode:2006AstL...32..759G,doi:10.1134/S1063773706110065,S2CID 119231169.
  7. ^abcdTetzlaff, N.; et al. (January 2011), "A catalogue of young runaway Hipparcos stars within 3 kpc from the Sun",Monthly Notices of the Royal Astronomical Society,410 (1):190–200,arXiv:1007.4883,Bibcode:2011MNRAS.410..190T,doi:10.1111/j.1365-2966.2010.17434.x,S2CID 118629873.
  8. ^abUnderhill, A. B.; et al. (November 1979), "Effective temperatures, angular diameters, distances and linear radii for 160 O and B stars",Monthly Notices of the Royal Astronomical Society,189 (3):601–605,Bibcode:1979MNRAS.189..601U,doi:10.1093/mnras/189.3.601
  9. ^abHohle, M. M.; et al. (April 2010), "Masses and luminosities of O- and B-type stars and red supergiants",Astronomische Nachrichten,331 (4): 349,arXiv:1003.2335,Bibcode:2010AN....331..349H,doi:10.1002/asna.200911355,S2CID 111387483.
  10. ^abcSoubiran, C.; et al. (June 2010), "The PASTEL catalogue of stellar parameters",Astronomy and Astrophysics,515: A111,arXiv:1004.1069,Bibcode:2010A&A...515A.111S,doi:10.1051/0004-6361/201014247,S2CID 118362423.
  11. ^abcStefl, S.; et al. (February 2010), "The 2008+ outburst of the Be star 28 CMa", in Rivinius, Th.; Curé, M. (eds.),The Interferometric View on Hot Stars, Revista Mexicana de Astronomía y Astrofísica, Serie de Conferencias, vol. 38, pp. 89–91,Bibcode:2010RMxAC..38...89S.
  12. ^"ome CMa".SIMBAD.Centre de données astronomiques de Strasbourg. Retrieved2017-09-03.
  13. ^Eggleton, P. P.; Tokovinin, A. A. (September 2008), "A catalogue of multiplicity among bright stellar systems",Monthly Notices of the Royal Astronomical Society,389 (2):869–879,arXiv:0806.2878,Bibcode:2008MNRAS.389..869E,doi:10.1111/j.1365-2966.2008.13596.x,S2CID 14878976.
  14. ^Štefl, S.; et al. (April 2003)."Stellar and circumstellar activity of the Be star ω CMa I. Line and continuum emission in 1996–2002"(PDF).Astronomy and Astrophysics.402:253–265.Bibcode:2003A&A...402..253S.doi:10.1051/0004-6361:20030224. Retrieved31 July 2022.
  15. ^Skiff, B. A. (October 2014), "Catalogue of Stellar Spectral Classifications",Lowell Observatory, VizieR On-line Data Catalog: B/mk,Bibcode:2014yCat....1.2023S.
  16. ^Ghoreyshi, M. R.; et al. (November 2016), "Modeling the Complete Lightcurve of ω CMa", in Sigut, T. A. A.; Jones, C. E. (eds.),Bright Emissaries: Be Stars as Messengers of Star-Disk Physics, Proceedings of a Meeting held at The University of Western Ontario, in London, Ontario, Canada, 11-13 August 2014, vol. 506, San Francisco:Astronomical Society of the Pacific, p. 315,arXiv:1506.08902,Bibcode:2016ASPC..506..315G.
  17. ^Harmanec, P. (June 1998), "On the nature of the Be phenomenon. I. The case of omega Canis Majoris",Astronomy and Astrophysics,334:558–570,Bibcode:1998A&A...334..558H.
  18. ^Štefl, S.; et al. (2000), "Tracing the Transient Periods in the Be Star 28 ω CMa", in Smith, Myron A.; Henrichs, Huib F. (eds.),The Be Phenomenon in Early-Type Stars, IAU Colloquium 175, ASP Conference Proceedings, vol. 214, Astronomical Society of the Pacific, p. 240,Bibcode:2000ASPC..214..240S,ISBN 1-58381-045-5.

External links

[edit]
Stars
Bayer
Flamsteed
Variable
HR
HD
Other
Exoplanets
Star
clusters
NGC
Other
Nebulae
Galaxies
NGC
Other
Astronomical events
Retrieved from "https://en.wikipedia.org/w/index.php?title=Omega_Canis_Majoris&oldid=1328240552"
Categories:
Hidden categories:
[8]ページ先頭
©2009-2026 Movatter.jp