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Title:
Presupernova evolution in massive interacting binaries
Authors:
Podsiadlowski, Ph.; Joss, P. C.; Hsu, J. J. L.
Affiliation:
AA(MIT, Cambridge, MA; Cambridge University Institute of Astronomy, England), AB(MIT, Cambridge, MA), AC(MIT, Cambridge, MA)
Publication:
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 391, no. 1, May 20, 1992, p. 246-264. (ApJ Homepage)
Publication Date:
05/1992
Category:
Astrophysics
Origin:
STI
NASA/STI Keywords:
BINARY STARS, MASSIVE STARS, STELLAR EVOLUTION, SUPERNOVAE, COMPUTATIONAL ASTROPHYSICS, MONTE CARLO METHOD, STELLAR ENVELOPES, STELLAR MASS ACCRETION, STELLAR MODELS, SUPERNOVA 1987A
DOI:
10.1086/171341
Bibliographic Code:
1992ApJ...391..246P

Abstract

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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