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 ⊙ 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 (Hawser-Feshbach). Some of the important ingredients are addressed. Discussed in more detail are approaches to predict level densities, parity distributions, and optical α-nucleus potentials.
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