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Nucleosynthesis in Stellar Explosions

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Part of the book series: Astrophysics and Space Science Library ((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.

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© 1984 D. Reidel Publishing Company

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Woosley, S.E., Axelrod, T.S., Weaver, T.A. (1984). Nucleosynthesis in Stellar Explosions. In: Chiosi, C., Renzini, A. (eds) Stellar Nucleosynthesis. Astrophysics and Space Science Library, vol 109. Springer, Dordrecht. https://doi.org/10.1007/978-94-009-6348-1_22

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  • DOI: https://doi.org/10.1007/978-94-009-6348-1_22

  • Publisher Name: Springer, Dordrecht

  • Print ISBN: 978-94-009-6350-4

  • Online ISBN: 978-94-009-6348-1

  • eBook Packages: Springer Book Archive

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