Nuclear data needs for the study of nucleosynthesis in massive stars
Author
Woosley, S.E.
Heger, A.
Rauscher, T.
Hoffman, R. D.
Attention
2299/11016
Abstract
The critical nuclear physics needed to calculate the evolution of and nucleosynthesis in massive stars is reviewed with emphasis on the uncertainties. Some reaction rates - the most important and uncertain still being C-12 (alpha, gamma)O-16 - are important for energy generation and stellar structure. Others, like Ne-22(alpha,n)Mg-25 and individual cross sections for neutron capture determine the overall yield and distribution of the s-process for elements lighter than A = 90. Still others affect the synthesis of individual nuclei, e.g., by the nu-process, the rp-process, and the gamma-process. Weak interaction rates are important in determining the structure of both the pre-collapse and the post-collapse supernova core. Finally, both the site for, and the nuclear physics of the r-process remains very uncertain, quite possibly because of the neglect of magnetic fields.