O-type main-sequence star


O-type main-sequence star

An O-type main-sequence star (O V) is a main-sequence (hydrogen-burning) star of spectral type O and luminosity class V. These stars have between 15 and 90 times the mass of the Sun and surface temperatures between 30,000 and 52,000 K. They are between 30,000 and 1,000,000 times as luminous as the Sun.[1][2] These stars are rare; it is estimated that there are no more than 20,000 in the entire Milky Way.[3] Examples include σ Orionis A and 10 Lacertae.[4][5]

See also

References

  1. ^ Tables 1 and 4, Fabrice Martins, Daniel Schaerer, and D. John Hiller (2005). "A new calibration of stellar parameters of Galactic O stars". Astronomy & Astrophysics 436: 1049–1065. arXiv:astro-ph/0503346. Bibcode 2005A&A...436.1049M. doi:10.1051/0004-6361:20042386. 
  2. ^ Table 5, William D. Vacca, Catharine D. Garmany, and J. Michael Shull (April 1996). "The Lyman-Continuum Fluxes and Stellar Parameters of O and Early B-Type Stars". Astrophysical Journal 460: 914–931. Bibcode 1996ApJ...460..914V. doi:10.1086/177020. 
  3. ^ Scientists Begin To Tease Out A Hidden Star's Secrets, ScienceDaily, July 27, 1998. Accessed on line November 13, 2007.
  4. ^ BD-02 1326A, SIMBAD query result. Accessed on line November 13, 2007.
  5. ^ 10 Lac, SIMBAD query result. Accessed on line November 13, 2007.

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