Evolution and nucleosynthesis of massive stars and related nuclear uncertainties

T. Rauscher

Research output: Contribution to journalArticlepeer-review

33 Citations (Scopus)
18 Downloads (Pure)

Abstract

Properties of atomic nuclei important for the prediction of astrophysical reaction rates are reviewed. In the first part, a recent simulation of evolution and nucleosynthesis of stars between 15 and 25 M-circle dot is presented. This study is used to illustrate the required nuclear input as well as to give examples of the sensitivity to certain rates. The second part focusses on the prediction of nuclear rates in the statistical model (Hauser-Feshbach). Some of the important ingredients are addressed. Discussed in more detail are approaches to predict level densities, parity distributions, and optical a-nucleus potentials.

Original languageEnglish
Pages (from-to)73C-89C
Number of pages17
JournalNuclear Physics A
Volume719
DOIs
Publication statusPublished - 19 May 2003
Event17th International Nuclear Physics Divisional Conference of the European-Physical-Society - DEBRECEN, Hungary
Duration: 30 Sept 20024 Oct 2002

Keywords

  • THERMONUCLEAR REACTION-RATES
  • SHELL
  • STATISTICAL-MODEL CALCULATIONS
  • SCATTERING
  • C-12(ALPHA,GAMMA)O-16
  • LEVEL DENSITIES
  • CAPTURE CROSS-SECTIONS
  • S-PROCESS
  • ASTROPHYSICALLY RELEVANT ENERGIES
  • O-18(ALPHA,GAMMA)NE-22

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