A binary evolutionary model for the progenitor of SN 1987 A

Details A binary evolutionary model for the progenitor of SN 1987 A A binary evolutionary model for the progenitor of SN 1987 A

Jul 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992a%26a...260..273d&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 260, no. 1-2, p. 273-282.

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Binary Stars, Stellar Evolution, Stellar Models, Supernova 1987A, Computational Astrophysics, Stellar Mass Accretion

Scientific paper

We explore the hypothesis that the blue progenitor of SN 1987 A was a component of a close binary. It is shown that a blue spectral appearance at the end of core helium burning (and possibly also during the following evolutionary phases) is a natural phenomenon for a star with initial mass between 9 and 15 solar masses which was originally in a close binary with mass ratio of about 1 and which accreted at least 8-10 solar masses while already being a hydrogen shell burning star. This phenomenon does not depend on the exact treatment of the convective core overshooting, the stellar wind mass loss rate, and the metallicity. A blue SN progenitor in the Galaxy would therefore not be a surprise.

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