Astronomy and Astrophysics – Astrophysics
Scientific paper
Jul 1978
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1978a%26a....67..373d&link_type=abstract
Astronomy and Astrophysics, vol. 67, no. 3, July 1978, p. 373-379. Research supported by the Fonds de la Recherche Fondamentale
Astronomy and Astrophysics
Astrophysics
90
Hot Stars, O Stars, Stellar Evolution, Stellar Mass Ejection, Stellar Winds, Wolf-Rayet Stars, Abundance, Helium, Hydrogen, Stellar Luminosity, X Ray Binaries
Scientific paper
Evolutionary tracks are computed for very massive stars (50, 60, 80, and 100 solar masses) with the inclusion of mass loss via stellar winds. The results are used in an attempt to explain the overluminosity observed in optical components of X-ray binaries, the occurrence of OBN stars, and the phenomenon of single Wolf-Rayet (WR) stars (types WN and WC). The calculations reveal that the overall evolutionary patterns of very massive (60-100 solar masses) and slightly less massive (20-50 solar masses) stars are similar, but that the more massive stars change their direction of evolution even before core hydrogen exhaustion, return to the ZAMS, and subsequently evolve toward the red-giant region. Comparisons with observations indicate that mass loss via a stellar wind may account for certain features of O and OBN stars as well as the overluminosity of early-type companions in X-ray binaries, that single WN stars might have evolved naturally from O stars with strong stellar winds and masses of 80 to 120 solar masses, and that single WR stars might actually be WR binaries composed of a pure helium star and a neutron-star companion.
de Greve Jean-Pierre
de Loore Camiel
Vanbeveren Dany
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