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

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 I1 supernova. Calculations were done for 15 Ma, 19 M,, 20 Ma, 21 Ma, and 25 Ma 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.