  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 solar masses 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) and direct capture (DWBA). Some of the important ingredients
are addressed. Discussed in more detail are approaches to predict level
densities, parity distributions, and optical alpha+nucleus potentials.
