Data needs for the astrophysical p-process

A status report is given on the experimental aspects of the astrophysical p-process that is responsible for the production of the heavy proton rich nuclei known as p-nuclei. The numerical modelling of the p-process scenario involves the knowledge of photodisintegration cross sections, mostly calculated through the Hauser-Feshbach statistical model approach. Recent experiments test the reliability of the model calculations in the proton rich region as well as providing indirect experimental information on the cross sections relevant to the p-process.