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Nucleosynthesis in Stellar Explosions

  • S. E. Woosley
  • Timothy S. Axelrod
  • Thomas A. Weaver
Part of the Astrophysics and Space Science Library book series (ASSL, volume 109)

Abstract

The final evolution and explosion of stars from 10 M⊙ to 106 M⊙ are reviewed with emphasis on factors affecting the expected nucleosynthesis. We order our paper in a sequence of decreasing mass. If, as many suspect, the stellar birth function was peaked towards larger masses at earlier times (see e.g., Silk 1977; but also see Palla, Salpeter, and Stahler 1983), this sequence of masses might also be regarded as a temporal sequence. At each stage of Galactic chemical evolution stars form from the ashes of preceding generations which typically had greater mass. A wide variety of Type I supernova models, most based upon accreting white dwarf stars, are also explored using the expected light curves, spectra, and nucleosynthesis as diagnostics. No clearly favored Type I model emerges that is capable of simultaneously satisfying all three constraints.

Keywords

Black Hole Light Curve Massive Star White Dwarf Helium Burning 
These keywords were added by machine and not by the authors. This process is experimental and the keywords may be updated as the learning algorithm improves.

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Copyright information

© D. Reidel Publishing Company 1984

Authors and Affiliations

  • S. E. Woosley
    • 1
    • 2
  • Timothy S. Axelrod
    • 3
  • Thomas A. Weaver
    • 4
  1. 1.Board of Studies in Astronomy and AstrophysicsUniversity of CaliforniaSanta CruzUSA
  2. 2.Special Studies Group, Lawrence Livermore National LaboratoryUniversity of CaliforniaLivermoreUSA
  3. 3.T-Division, Lawrence Livermore National LaboratoryUniversity of CaliforniaLivermoreUSA
  4. 4.Special Studies Group, Lawrence Livermore National LaboratoryUniversity of CaliforniaLivermoreUSA

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