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Progenitors and Hydrodynamics of Type II and lb Supernovae

Published online by Cambridge University Press:  12 April 2016

S. E. Woosley ,
T. A. Weaver  and
R. G. Eastman
S. E. Woosley
Affiliation:
Board of Studies in Astronomy and Astrophysics, UCO/Lick Observatory, UCSC, Santa Cruz CA 95064, USA General Studies Group, Physics Department, Lawrence Livermore National Laboratory, Livermore, CA 94550, USA
T. A. Weaver
Affiliation:
General Studies Group, Physics Department, Lawrence Livermore National Laboratory, Livermore, CA 94550, USA
R. G. Eastman
Affiliation:
Board of Studies in Astronomy and Astrophysics, UCO/Lick Observatory, UCSC, Santa Cruz CA 95064, USA

Abstract

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We review critical physics affecting the observational characteristics of those supernovae that occur in massive stars. Particular emphasis is given to 1) how mass loss, either to a binary companion or by a radiatively driven wind, affects the type and light curve of the supernova, and 2) the interaction of the outgoing supernova shock with regions of increasing pr3 in the stellar mantle. One conclusion is that Type II-L supernovae may occur in mass exchanging binaries very similar to the one that produced SN 1993J, but with slightly larger initial separations and residual hydrogen envelopes (∼1 Mʘ and radius ∼ several AU). The shock interaction, on the other hand, has important implications for the formation of black holes in explosions that are, near peak light, observationally indistinguishable from ordinary Type II-p and lb supernovae.

Type
Type lb and Type II Supernovae
Information
International Astronomical Union Colloquium , Volume 145: Supernovae and Supernova Remnants , 1996 , pp. 137 - 147
Copyright
Copyright © Cambridge University Press 1996

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