An overview will be given on reaction rates for the astrophysical p-process responsible for the production of the heavy proton rich nuclei known as p-nuclei.
The nuclear physics input of the standard p-process scenario (gamma-process) involves the knowledge of photo induced reaction cross sections, mostly calculated within the Hauser-Feshbach statistical model [1,2].
Experimentally determined radiative capture cross section data can test the reliability of the model calculations in the proton rich region as well as provide experimental information directly relevant to the p-process. Recent advances involving also the study of (p,n) reactions underline the importance of the stellar enhancement factor and call for a modified optical parameter set [3,4].
In addition, complementary low energy elastic alpha scattering experiments can serve as a tool todetermine alpha optical potentials, an important and relatively poorly known ingredient of statistical model calculations.
ATOMKI has a long range program, supported by the European Research Council, to study reactions relevant to p-process using low energy accelerators. A full description of the scientific program, its advances and limitations will be provided.
[1] M. Arnould and S. Goriely, Phys. Rep. 384 (2003) 1.
[2] T. Rauscher and F.-K. Thielemann, At. Data Nucl. Data Tables 75, (2000) 1.
[3] G.G. Kiss et al., Phys. Rev. C76 (2007) 5807.
[4] G.G. Kiss et al., Phys. Rev. Lett. 101 (2008) 191101.
