Nuclear input for the p-process

To properly describe the astrophysical p-process, both the stellar environment and the complete nuclear input are needed. The stellar environment most favored to-date is the O/Ne layer of a 25 solar mass type II supernova. The nuclear input requires reaction rates for about 20,000 reaction involving nearly 2,000 nuclei. A vast majority of the reactions is calculated using Hauser-Feshbach statistical models and only a small fraction has been verified experimentally. Here, impact of various parameters of the HF models on the prediction of the production of the p-nuclei is presented.