Omega Carinae

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This article is about ω Carinae and is not to be confused with w Carinae.
ω Carinae
Location of ω Carinae (circled)
Observation data
Epoch J2000      Equinox J2000
Constellation Carina[1]
Right ascension 10h 13m 44.21739s[2]
Declination −70° 02′ 16.4563″[2]
Apparent magnitude (V) 3.29[3]
Characteristics
Spectral type B8 IIIe[4]
U−B color index −0.285[5]
B−V color index −0.083[5]
Astrometry
Radial velocity (Rv)+7.0[3] km/s
Proper motion (μ) RA: −36.01 mas/yr[2]
Dec.: +7.09 mas/yr[2]
Parallax (π)9.54±0.09 mas[2]
Distance342 ± 3 ly
(104.8 ± 1.0 pc)
Absolute magnitude (MV)−1.81[1]
Details
Mass4.9[6] M☉
Radius7.20±0.14[7] R☉
Luminosity918[8] L☉
Surface gravity (log g)3.51[8] cgs
Temperature11,630[8] K
Rotational velocity (v sin i)240[8] km/s
Other designations
ω Car, CD−69°1178, FK5 385, HD 89080, HIP 50099, HR 4037, SAO 250885[9]
Database references
SIMBADdata

Omega Carinae is a star in the constellation Carina. Its name is a Bayer designation that is Latinized from ω Carinae, and abbreviated Omega Car or ω Car. With a declination greater than 70 degrees south of the celestial equator, it is the most southerly of the bright stars of Carina (third-magnitude or brighter), and it is part of a southern asterism known as the Diamond Cross. This naked eye star has an apparent visual magnitude of 3.3 and is located at a distance of about 342 light-years (105 parsecs) from Earth.

Properties

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Omega Carinae has a stellar classification of B8 IIIe,[4] which places it in the category of Be stars, that display emission lines of hydrogen their spectrum. Omega Carinae is a shell star,[4] having a circumstellar disk of gas surrounding its equator. The luminosity class of III indicates it has evolved into a giant star, having exhausted the hydrogen at its core and left the main sequence. The effective temperature of 11,630 K[8] in its outer envelope is what gives this star the blue-white hue that is characteristic of B-type stars.

This star is rotating rapidly with a projected rotational velocity of 240 km/s,[8] which gives a lower limit to the star's azimuthal velocity along the equator. The critical equatorial velocity, at which the star would begin to break up, is 320 km s−1. The star's axis of rotation is inclined by an estimated angle of 70.8° to the line of sight from the Earth.[10]

In the next 7500 years, the south Celestial pole will pass close to this star (AD 5800) and then I Carinae.[11]

In culture

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In Chinese, 南船 (Nán Chuán), meaning Southern Boat, refers to an asterism consisting of ω Carinae, V337 Carinae, PP Carinae, θ Carinae and β Carinae .[12] Consequently, ω Carinae itself is known as 南船四 (Nán Chuán sì, English: the Fourth Star of Southern Boat.)[13]

References

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  1. ^ a b Anderson, 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 at VizieR.
  2. ^ a b c d van Leeuwen, F. (November 2007), "Validation of the new Hipparcos reduction", Astronomy and Astrophysics, 474 (2): 653–664, arXiv:0708.1752, Bibcode:2007A&A...474..653V, doi:10.1051/0004-6361:20078357, S2CID 18759600.
  3. ^ a b Wielen, R.; et al. (1999), "Sixth Catalogue of Fundamental Stars (FK6). Part I. Basic fundamental stars with direct solutions", Veroeffentlichungen des Astronomischen Rechen-Instituts Heidelberg, 35 (35), Astronomisches Rechen-Institut Heidelberg: 1, Bibcode:1999VeARI..35....1W.
  4. ^ a b c Rivinius, Th.; et al. (November 2006), "Bright Be-shell stars", Astronomy and Astrophysics, 459 (1): 137–145, Bibcode:2006A&A...459..137R, doi:10.1051/0004-6361:20053008.
  5. ^ a b Gutierrez-Moreno, Adelina; Moreno, Hugo (June 1968), "A photometric investigation of the Scorpio-Centaurus association", Astrophysical Journal Supplement, 15: 459, Bibcode:1968ApJS...15..459G, doi:10.1086/190168.
  6. ^ Quintana, Alexis L.; Wright, Nicholas J.; Martínez García, Juan (2025), "A census of OB stars within 1 KPC and the star formation and core collapse supernova rates of the Milky Way", Monthly Notices of the Royal Astronomical Society, 538 (3): 1367, arXiv:2503.08286, Bibcode:2025MNRAS.538.1367Q, doi:10.1093/mnras/staf083.
  7. ^ Arcos, C.; Kanaan, S.; Chávez, J.; Vanzi, L.; Araya, I.; Curé, M. (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, arXiv:1711.08675, Bibcode:2018MNRAS.474.5287A, doi:10.1093/mnras/stx3075.
  8. ^ a b c d e f Zorec, J.; et al. (2016), "Critical study of the distribution of rotational velocities of be stars. I. Deconvolution methods, effects due to gravity darkening, macroturbulence, and binarity", Astronomy and Astrophysics, 595: A132, Bibcode:2016A&A...595A.132Z, doi:10.1051/0004-6361/201628760, hdl:11336/37946.
  9. ^ "ome Car", SIMBAD, Centre de données astronomiques de Strasbourg, retrieved 2012-01-13.
  10. ^ Frémat, Y.; et al. (September 2005), "Effects of gravitational darkening on the determination of fundamental parameters in fast-rotating B-type stars", Astronomy and Astrophysics, 440 (1): 305–320, arXiv:astro-ph/0503381, Bibcode:2005A&A...440..305F, doi:10.1051/0004-6361:20042229, S2CID 19016751.
  11. ^ Kieron Taylor (2005), "Precession", moonkmft, retrieved 2020-01-19.
  12. ^ (in Chinese) 中國星座神話, written by 陳久金. Published by 台灣書房出版有限公司, 2005, ISBN 978-986-7332-25-7.
  13. ^ (in Chinese) AEEA (Activities of Exhibition and Education in Astronomy) 天文教育資訊網 2006 年 7 月 28 日 Archived 2013-05-13 at the Wayback Machine
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