Hydrostatic and explosive nucleosynthesis in massive stars using improved nuclear and stellar physics

T. Rauscher, A. Heger, R. D. Hoffman, S.E. Woosley

Research output: Contribution to journalArticlepeer-review

11 Citations (Scopus)

Abstract

We have performed the first calculations to follow the evolution of all stable nuclei and their radioactive progenitors in a finely-zoned stellar model computed from the onset of central hydrogen burning through explosion as a Type 11 supernova. Calculations were done for 15 M-circle dot, 19 M-circle dot, 20 Mcircle dot, 21 Mcircle dot, and 25 Mcircle dot Pop I stars using the most recently available set of experimental and theoretical nuclear data, revised opacity tables, and taking into account mass loss due to stellar winds. Here, we focus on the nuclear inputs.

Original languageEnglish
Pages (from-to)463C-465C
Number of pages3
JournalNuclear Physics A
Volume718
DOIs
Publication statusPublished - 5 May 2003
Event7th International Symposium on Nuclei in the Cosmos (NIC7) - FUJI, Japan
Duration: 8 Jul 200212 Jul 2002

Keywords

  • THERMONUCLEAR REACTION-RATES
  • MODEL CALCULATIONS
  • CROSS-SECTIONS
  • BEAM
  • O-18(ALPHA,GAMMA)NE-22

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