Single Stars and Supernovae from Wolf-Rayet Secondaries

Details Single Stars and Supernovae from Wolf-Rayet Secondaries Single Stars and Supernovae from Wolf-Rayet Secondaries

Oct 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005aipc..797..549d&link_type=abstract

INTERACTING BINARIES: Accretion, Evolution, and Outcomes. AIP Conference Proceedings, Volume 797, pp. 549-552 (2005).

Computer Science

1

Wolf-Rayet Stars, Binary Stars, Supernovae, Stellar Evolution, Emission-Line Stars, Binary And Multiple Stars, Supernovae, Stellar Structure, Interiors, Evolution, Nucleosynthesis, Ages

Scientific paper

We investigate the population of single Wolf-Rayet (WR) stars in the Milky Way and Magellanic Clouds which may have resulted from massive binary evolution. Observationally, the binary fraction amongst Wolf-Rayet stars is much smaller than that of O stars, their direct progenitors, suggesting that many single WR stars might once have been part of a binary system. We present a grid of stellar models aimed at studying the evolution of the secondary in the case that the supernova explosion of the primary unbinds the binary to see if a suitable population may be produced in this manner. Whilst transferring a significant amount of mass between the stars in such a system is difficult to achieve - a contact binary often resulting instead - the accretion of He-enriched matter onto those secondaries which avoid contact changes their subsequent evolution in a more complex manner than simple rejuvenation and increases the liklihood that they will subsequently undergo a WR phase. If the initial binary fraction is high, a significant population of single WR stars and type Ib/c supernovae could be produced by this seemingly unlikely route.

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