Binary progenitors of supernovae

Details Binary progenitors of supernovae Binary progenitors of supernovae

Dec 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984japa....5..389t&link_type=abstract

Journal of Astrophysics and Astronomy (ISSN 0250-6335), vol. 5, Dec. 1984, p. 389-402.

Astronomy and Astrophysics

Astrophysics

9

Binary Stars, Stellar Evolution, Supernovae, Cataclysmic Variables, Companion Stars, Hydrogen, Neutron Stars, Stellar Envelopes, White Dwarf Stars

Scientific paper

Among the massive stars that are expected to produce Type II, hydrogen-rich supernovae, the presence of a close companion can increase the main sequence mass needed to yield a collapsing core. In addition, due to mass transfer from the primary to the secondary, the companion enhances the stripping of the stellar hydrogen envelope produced by single star winds and thereby makes it harder for the star to give rise to a typical SN II light curve. Among the less massive stars that may be the basis for Type I, hydrogen-free supernovae, a close companion could be an innocent bystander to carbon detonation/deflagration in the primary. It may alternatively be a vital participant which transfers material to a white dwarf primary and drives it to explosive conditions.

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