Interacting massive binaries, H-R diagram of the Large Magellanic Cloud, and SN 1987A

Details Interacting massive binaries, H-R diagram of the Large Magellanic Cloud, and SN 1987A Interacting massive binaries, H-R diagram of the Large Magellanic Cloud, and SN 1987A

Jul 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993apj...411..848r&link_type=abstract

Astrophysical Journal - Part 1 (ISSN 0004-637X), vol. 411, no. 2, p. 848-863.

Astronomy and Astrophysics

Astrophysics

2

Binary Stars, Hertzsprung-Russell Diagram, High Energy Interactions, Magellanic Clouds, Massive Stars, Supernova 1987A, Blue Stars, Stellar Evolution, Stellar Models, Supergiant Stars

Scientific paper

It is shown that the standard physical inputs used in single star evolutionary models do not give good agreement with observational constraints on massive star models for the LMC. The effect of helium enrichment of secondary stars in binary systems and the presence of a substantial fraction of such stars in the blue supergiant (BSG) region is explored. It is shown that the resulting distribution of stars in the BSG region gives good agreement with all the observational features. We show that mass transfer to the secondary while it is still within its main sequence could give an evolutionary model at 20 solar masses which stays in the blue throughout its lifetime and yet could show helium enrichment and CNO processing in the circumstellar material and the envelope of the star consistent with the observations of SN 1987A. It is argued, however, that a more consistent model for the progenitor star is obtained if the component masses in the binary system are nearly equal and the secondary star accretes matter from the primary after it evolves to the Hayashi track. The presence of highly helium- and nitrogen-enriched stars in the BSG region is shown to arise as a natural consequence of interacting binary star evolution.

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