Astronomy:Kappa Canis Majoris

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Short description: Star in the constellation Canis Major
Kappa Canis Majoris
Location of κ Canis Majoris (circled)
Observation data
Equinox J2000.0]] (ICRS)
Constellation Canis Major
Right ascension  06h 49m 50.45933s[1]
Declination −32° 30′ 30.5225″[1]
Apparent magnitude (V) +3.87[2]
Characteristics
Spectral type B1.5 Ve[3]
U−B color index −0.97[2]
B−V color index −0.20[2]
Variable type γ Cas[3]
Astrometry
Radial velocity (Rv)+14.0±4.1[4] km/s
Proper motion (μ) RA: −8.84[1] mas/yr
Dec.: +3.73[1] mas/yr
Parallax (π)4.95 ± 0.12[1] mas
Distance660 ± 20 ly
(202 ± 5 pc)
Absolute magnitude (MV)−3.03[5]
Details
Mass12.2±0.3[6] M☉
Radius5.9[7] R☉
Luminosity (bolometric)18,876[8] L☉
Surface gravity (log g)4.07[7] cgs
Temperature24,600[7] K
Rotational velocity (v sin i)290±6[9] km/s
Age13.3±1.2[6] Myr
Other designations
κ CMa, 13 Canis Majoris, CD−32°3404, FK5 1180, GC 8946, HD 50013, HIP 32759, HR 2538, SAO 197258[10]
Database references
SIMBADdata

Kappa Canis Majoris is a solitary,[11] blue-white hued star in the constellation Canis Major. Its name is a Bayer designation that is Latinized from κ Canis Majoris, and abbreviated Kappa CMa or κ CMa. This star is visible to the naked eye with an apparent visual magnitude of +3.87.[2] Based upon an annual parallax shift of 7.70 mas as seen from Earth,[1] this star is located about 660 light years from the Sun. It is receding from the Sun with a line of sight velocity of +14 km/s.[4]

File:KappaCMaLightCurve.png
A light curve for Kappa Canis Majoris. The main plot, from Hipparcos data,[12] shows the long-term variability and the inset plot, from TESS data,[13] shows the short-term variability.

This is a massive B-type main-sequence star with a stellar classification of B1.5 Ve,[3] although Hiltner et al. (1969) classified it as B1.5 IVe[14] suggesting it is a subgiant star. The 'e' suffix indicates it is a rapidly rotating Be star with a circumstellar decretion disk of heated gas.[7] The radius of the emitting disk is about 0.20±0.06 astronomical unit|AU, or about 3.7 times the radius of the star.[15] It is classified as a Gamma Cassiopeiae type variable star and its brightness varies from magnitude +3.4 to +3.97.[3] The star became 50% brighter between 1963 and 1978, increasing from magnitude 3.96 or so to 3.52.[16]

This star is about 13.3[6] million years old and spinning with a projected rotational velocity of 290 km/s.[9] It has 6 times the radius of the Sun and 12 times the Sun's mass. The star is emitting 18,876[8] times the luminosity of the Sun from its photosphere at an effective temperature of 24,600 K.[7]

Naming

In Chinese, 弧矢 (Hú Shǐ), meaning Bow and Arrow,[17] refers to an asterism consisting of κ Canis Majoris, δ Canis Majoris, η Canis Majoris, HD 63032, HD 65456, ο Puppis, k Puppis, ε Canis Majoris and π Puppis. Consequently, κ Canis Majoris itself is known as 弧矢八 (Hú Shǐ bā, English: the Eighth Star of Bow and Arrow.)[18]

References

  1. ↑ 1.0 1.1 1.2 1.3 1.4 1.5 van Leeuwen, F. (2007), "Validation of the new Hipparcos reduction", Astronomy and Astrophysics 474 (2): 653–664, doi:10.1051/0004-6361:20078357, Bibcode: 2007A&A...474..653V. 
  2. ↑ 2.0 2.1 2.2 2.3 Feinstein, A.; Marraco, H. G. (November 1979), "The photometric behavior of Be Stars", Astronomical Journal 84: 1713–1725, doi:10.1086/112600, Bibcode: 1979AJ.....84.1713F. 
  3. ↑ 3.0 3.1 3.2 3.3 Watson, Christopher (January 4, 2010), "Kappa Canis Majoris", AAVSO Website (American Association of Variable Star Observers), http://www.aavso.org/vsx/index.php?view=detail.top&oid=5508, retrieved 2014-02-24. 
  4. ↑ 4.0 4.1 de Bruijne, J. H. J.; Eilers, A.-C. (October 2012), "Radial velocities for the HIPPARCOS-Gaia Hundred-Thousand-Proper-Motion project", Astronomy & Astrophysics 546: 14, doi:10.1051/0004-6361/201219219, A61, Bibcode: 2012A&A...546A..61D. 
  5. ↑ Anderson, E.; Francis, Ch. (2012), "XHIP: An extended hipparcos compilation", Astronomy Letters 38 (5): 331, doi:10.1134/S1063773712050015, Bibcode: 2012AstL...38..331A. 
  6. ↑ 6.0 6.1 6.2 Tetzlaff, 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, doi:10.1111/j.1365-2966.2010.17434.x, Bibcode: 2011MNRAS.410..190T. 
  7. ↑ 7.0 7.1 7.2 7.3 7.4 Meilland, A. et al. (October 2009), "VLTI/MIDI observations of 7 classical Be stars", Astronomy and Astrophysics 505 (2): 687–693, doi:10.1051/0004-6361/200911960, Bibcode: 2009A&A...505..687M. 
  8. ↑ 8.0 8.1 Hohle, M. M. et al. (April 2010), "Masses and luminosities of O- and B-type stars and red supergiants", Astronomische Nachrichten 331 (4): 349, doi:10.1002/asna.200911355, Bibcode: 2010AN....331..349H. 
  9. ↑ 9.0 9.1 Arcos, C. et al. (March 2018), "Stellar parameters and H-α line profile variability of Be stars in the BeSOS survey", Monthly Notices of the Royal Astronomical Society 474 (4): 5287–5299, doi:10.1093/mnras/stx3075, Bibcode: 2018MNRAS.474.5287A. 
  10. ↑ "kap CMa". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=kap+CMa. 
  11. ↑ 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, doi:10.1111/j.1365-2966.2008.13596.x, Bibcode: 2008MNRAS.389..869E. 
  12. ↑ Hipparcos Tools Interactive Data Access, ESA, https://www.cosmos.esa.int/web/hipparcos/interactive-data-access, retrieved 8 December 2021. 
  13. ↑ MAST: Barbara A. Mikulski Archive for Space Telescopes, Space Telescope Science Institute, https://mast.stsci.edu/portal/Mashup/Clients/Mast/Portal.html, retrieved 8 December 2021. 
  14. ↑ Hiltner, W. A. et al. (July 1969), "MK Spectral Types for Bright Southern OB Stars", Astrophysical Journal 157: 313–326, doi:10.1086/150069, Bibcode: 1969ApJ...157..313H. 
  15. ↑ Rivinius, Thomas et al. (2013), "Classical Be stars. Rapidly rotating B stars with viscous Keplerian decretion disks", The Astronomy and Astrophysics Review 21: 69, doi:10.1007/s00159-013-0069-0, Bibcode: 2013A&ARv..21...69R. 
  16. ↑ Kaler, James B. (March 1, 2013), "Kappa Canis Majoris", Stars (University of Illinois), http://stars.astro.illinois.edu/sow/kappacma.html, retrieved 2014-02-24. 
  17. ↑ 弧矢 (Hú Shǐ) is westernized into Koo She. R.H. Allen had opinion that Koo She refers to the asterism including δ Velorum and ω Velorum. AEEA opinion is, δ Velorum is member of 天社 (Tiān Shè), meaning Celestial Earth God's Temple asterism and ω Velorum is not member of any asterisms. 天社 (Tiān Shè) is westernized into Tseen She and R.H.Allen used the term Tseen She for Chinese name of η Carinae. See Richard Hinckley Allen: Star Names — Their Lore and Meaning: Argo Navis and Script error: The function "in_lang" does not exist. AEEA (Activities of Exhibition and Education in Astronomy) 天文教育資訊網 2006 年 7 月 17 日 .
  18. ↑ Script error: The function "in_lang" does not exist. AEEA (Activities of Exhibition and Education in Astronomy) 天文教育資訊網 2006 年 7 月 17 日



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