Back نجم أزرق فائق العملقة Arabic Superxigante azul AST নীল অতিদানব তারা Bengali/Bangla Supergegant blau Catalan Modrý veleobr Czech Сенкер вышкайсăр гигант CV Blua supergiganto Esperanto Supergigante azul Spanish Supererraldoi urdin Basque ابرغول آبی Persian

Blue supergiant

A blue supergiant (BSG) is a hot, luminous star, often referred to as an OB supergiant. They are usually considered to be those with luminosity class I and spectral class B9 or earlier,[1] although sometimes A-class supergiants are also deemed blue supergiants.[2][3]

Blue supergiants are found towards the top left of the Hertzsprung–Russell diagram, above and to the right of the main sequence. They are larger than the Sun but smaller than a red supergiant, with surface temperatures of 10,000–50,000 K and luminosities from about 10,000 to a million times that of the Sun. They are most often an evolutionary phase between high-mass, hydrogen-fusing main-sequence stars and helium-fusing red supergiants, although new research suggests they could be the result of stellar mergers.[4][5]

The majority of supergiants are also blue (B-type) supergiants; blue supergiants from classes O9.5 to B2 are even more common than their main sequence counterparts.[6] More post-main-sequence blue supergiants are observed than what is expected from theoretical models, which expect blue supergiants to be short-lived. This results in the blue supergiant problem, although unusual stellar interiors (such as hotter blue supergiants having oversized hydrogen-fusing cores and cooler ones having undersized helium-fusing cores) may explain this.[7]

  1. ^ Massey, P.; Puls, J.; Pauldrach, A. W. A.; Bresolin, F.; Kudritzki, R. P.; Simon, T. (2005). "The Physical Properties and Effective Temperature Scale of O-Type Stars as a Function of Metallicity. II. Analysis of 20 More Magellanic Cloud Stars and Results from the Complete Sample". The Astrophysical Journal. 627 (1): 477–519. arXiv:astro-ph/0503464. Bibcode:2005ApJ...627..477M. doi:10.1086/430417. S2CID 18172086.
  2. ^ Yüce, Kutluay (2005-01-01). "Spectral Analysis of 4 Lacertae and ν Cephei". Baltic Astronomy. 14: 51–82. Bibcode:2005BaltA..14...51Y. ISSN 1021-6766.
  3. ^ Burgos, A. de; Simon-Díaz, S.; Lennon, D. J.; Dorda, R.; Negueruela, I.; Urbaneja, M. A.; Patrick, L. R.; Herrero, A. (2020-11-01). "High-resolution spectroscopic study of massive blue and red supergiants in Perseus OB1 - I. Definition of the sample, membership, and kinematics". Astronomy & Astrophysics. 643: A116. arXiv:2008.13299. Bibcode:2020A&A...643A.116D. doi:10.1051/0004-6361/202039019. ISSN 0004-6361.
  4. ^ Menon, Athira; Ercolino, Andrea; Urbaneja, Miguel A.; Lennon, Daniel J.; Herrero, Artemio; Hirai, Ryosuke; Langer, Norbert; Schootemeijer, Abel; Chatzopoulos, Emmanouil; Frank, Juhan; Shiber, Sagiv (March 2024). "Evidence for Evolved Stellar Binary Mergers in Observed B-type Blue Supergiants". The Astrophysical Journal Letters. 963 (2): L42. Bibcode:2024ApJ...963L..42M. doi:10.3847/2041-8213/ad2074. ISSN 2041-8205.
  5. ^ Cite error: The named reference :1 was invoked but never defined (see the help page).
  6. ^ Sowell, J. R.; Trippe, M.; Caballero-Nieves, S. M.; Houk, N. (2007-07-18). "H-R Diagrams Based on the HD Stars in the Michigan Spectral Catalogue and the Hipparcos Catalog". The Astronomical Journal. 134 (3): 1089. Bibcode:2007AJ....134.1089S. doi:10.1086/520060. ISSN 1538-3881.
  7. ^ Bellinger, Earl Patrick; de Mink, Selma E.; van Rossem, Walter E.; Justham, Stephen (2023-10-31). "The Potential of Asteroseismology to Resolve the Blue Supergiant Problem". arXiv:2311.00038 [astro-ph.SR].
From Wikipedia, the free encyclopedia · View on Wikipedia

Developed by Nelliwinne