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Radiation Hydrodynamics in Stars and Compact Objects pp 91–120Cite as

The physics of supernovae

  • 3. Supernovae
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Part of the book series: Lecture Notes in Physics ((LNP,volume 255))

Abstract

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.

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Authors and Affiliations

  1. Board of Studies in Astronomy and Astrophysics Lick Observatory, University of California at Santa Cruz, 95064, Santa Cruz, CA

    S. E. Woosley

  2. Special Studies Group, Lawrence Livermore National Laboratory, 94550, Livermore, CA

    S. E. Woosley & Thomas A. Weaver

Authors
  1. S. E. Woosley
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  2. Thomas A. Weaver
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Dimitri Mihalas Karl-Heinz A. Winkler

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© 1986 Springer-Verlag

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Woosley, S.E., Weaver, T.A. (1986). The physics of supernovae. In: Mihalas, D., Winkler, KH.A. (eds) Radiation Hydrodynamics in Stars and Compact Objects. Lecture Notes in Physics, vol 255. Springer, Berlin, Heidelberg. https://doi.org/10.1007/3-540-16764-1_7

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  • DOI: https://doi.org/10.1007/3-540-16764-1_7

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  • Print ISBN: 978-3-540-16764-8

  • Online ISBN: 978-3-540-38739-8

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