Astronomy and Astrophysics – Astrophysics
Scientific paper
Oct 1982
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982a%26a...114..409m&link_type=abstract
Astronomy and Astrophysics, vol. 114, no. 2, Oct. 1982, p. 409-413.
Astronomy and Astrophysics
Astrophysics
42
Stellar Evolution, Stellar Mass Ejection, Supernovae, Wolf-Rayet Stars, Stellar Models, Stellar Structure
Scientific paper
The evolution of stars more massive than nine solar masses is similar for models with mass loss at the observed rates and models of constant mass, indicating that the final outcome of the centers of OB stars is not substantially modified by stellar winds. Most mass-losing OB stars that may after several stages become WR stars are therefore likely to explode as supernovae. A fraction of such stars may, however, end their life as small mass planetary nuclei. Three different determinations are made of the fraction of supernovae originating from WR progenitors. The first estimate is based on the approximately 1200 WR stars in the Galaxy, the second on the supernova remnants, and the third on current mass spectrum and mass limits. The three estimates are consistent and indicate one supernova from a WR progenitor over 3-7 supernova events.
Lequeux James
Maeder Andre
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