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Type II Supernovae

  • Chapter
Problems of Collapse and Numerical Relativity

Part of the book series: NATO ASI Series ((ASIC,volume 134))

Abstract

Evidence is briefly reviewed for believing that the core bounce mechanism actually gives rise to Type II supernovae in massive stars. Strongest evidence comes from the historical observation of the Crab Nebula light curve, the existence of pulsars, and from the nucleosynthesis of a few very neutron-rich isotopes such as 48Ca. A new presupernova model for a 25 M⊙ star is presented which has an iron core mass at the time of collapse that is smaller than in our previous studies. The evolution of a Population III (Z = 0) 25 M⊙ star (currently evolved up to the point of silicon shell burning) is also briefly reviewed and implications for nucleosynthesis discussed. It is pointed out that the explosion of relatively compact stars such as the Population III 25 M⊙ model or Wolf-Rayet stars devoid of any hydrogen envelope is not likely to produce either a brilliant optical display or a spectrum similar to common Type II events. Such explosions may have escaped detection.

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Author information

Authors and Affiliations

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

    S. E. Woosley

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

    S. E. Woosley & Thomas A. Weaver

Authors
  1. S. E. Woosley
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  2. Thomas A. Weaver
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Editor information

Editors and Affiliations

  1. Université Paul Sabatier, Toulouse, France

    Daniel Bancel

  2. Observatoire de Meudon, Meudon, France

    Monique Signore

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© 1984 D. Reidel Publishing Company

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Woosley, S.E., Weaver, T.A. (1984). Type II Supernovae. In: Bancel, D., Signore, M. (eds) Problems of Collapse and Numerical Relativity. NATO ASI Series, vol 134. Springer, Dordrecht. https://doi.org/10.1007/978-94-009-6460-0_2

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  • DOI: https://doi.org/10.1007/978-94-009-6460-0_2

  • Publisher Name: Springer, Dordrecht

  • Print ISBN: 978-94-009-6462-4

  • Online ISBN: 978-94-009-6460-0

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