Binary progenitors of Supernovae |
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Authors: | Virginia Trimble |
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Institution: | (1) Department of Physics, University of California, 92717 Irvine, CA, USA;(2) Astronomy Program, University of Maryland, 20742 College Park, MD, USA |
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Abstract: | Supernovae of both Type I (hydrogen-poor) and Type II (hydrogen-rich) can be expected to occur among binary stars. Among massive
stars (>10 M•), the companion makes it more difficult for the primary to develop an unstable core of >1.4.M• while still retaining
the extended, hydrogen-rich envelope needed to make a typical Type II light curve. Among 1–10 M• stars, on the other hand,
a companion plays a vital role in currently popular models for Type I events, by transferring material to the primary after
it has become a stable white dwarf, and so driving it to conditions where either core collapse or explosive nuclear burning
will occur. Several difficulties (involving nucleosynthesis, numbers and lifetimes of progenitors, the mass-transfer mechanism,etc.) still exist in these models. Some of them are overcome by a recent, promising scenario in which the secondary also evolves
to a degenerate configuration, and the two white dwarfs spiral together to produce a hydrogen-free explosion, long after single
stars of the same initial masses have ceased to be capable of fireworks. |
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Keywords: | Supernovae progenitors binary stars evolution |
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