Presupernova evolution in massive interacting binaries

Details Presupernova evolution in massive interacting binaries Presupernova evolution in massive interacting binaries

May 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992apj...391..246p&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 391, no. 1, May 20, 1992, p. 246-264.

Statistics

Computation

192

Binary Stars, Massive Stars, Stellar Evolution, Supernovae, Computational Astrophysics, Monte Carlo Method, Stellar Envelopes, Stellar Mass Accretion, Stellar Models, Supernova 1987A

Scientific paper

The way in which binary interaction affects the presupernova evolution of massive close binaries and the resulting supernova explosions is investigated systematically by means of a Henyey-type stellar evolution code that was modified to allow its application to binary stellar evolution calculations. The code makes it possible to trace the effects of mass and angular momentum loss from the binary, as well as mass transfer within the binary system. It is found that a large number of binary scenarios can be distinguished, depending on the type of binary interaction and the evolutionary stage of the supernova progenitor at the time of the interaction. Monte Carlo simulations are performed to estimate the frequencies of the occurrence of various scenarios. It is found that, because of a previous binary interaction, 15-30 percent of all massive stars (with initial masses greater than about 8 solar masses) become helium stars, and another 5 percent of all massive stars end their lives as blue supergiants rather than as red supergiants.

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