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The Physics of Supernovae

Published online by Cambridge University Press:  12 April 2016

S.E. Woosley  and
Thomas A. Weaver
S.E. Woosley
Affiliation:
Board of Studies in Astronomy and Astrophysics Lick Observatory, University of California at Santa Cruz, Santa Cruz CA 95064 and Special Studies Group, Lawrence Livermore National Laboratory, Livermore CA 94550
Thomas A. Weaver
Affiliation:
Special Studies Group, Lawrence Livermore National Laboratory, University of California, Livermore CA 94550

Abstract

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Presupernova models of massive stars are presented and their explosion by “delayed neutrino transport” examined. A new form of long duration Type II supernova model is also explored based upon repeated encounter with the electron-positron pair instability in stars heavier than about 60 M⊙. Carbon deflagration in white dwarfs is discussed as the probable explanation of Type I supernovae and special attention is paid to the physical processes whereby a nuclear flame propagates through degenerate carbon.

Information

Type
3. Supernovae
Information
International Astronomical Union Colloquium , Volume 89: Radiation Hydrodynamics in Stars and Compacts Objects , 1986 , pp. 90 - 120
Copyright
Copyright © Springer-Verlag 1986

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