Sensitivity of p-Nuclei to (n,g) Reaction Rates

The astrophysical \emph{p}-process, which is responsible for the creation of the proton-rich \emph{p}-nuclei, is still not well understood. A sensitivity study of \emph{p}-nuclei abundances to (\emph{n,$\gamma$}) and (\emph{$\gamma$,n}) reaction rates was conducted at the National Superconducting Cyclotron Laboratory using a nuclear reaction network created at Clemson University. This network simulates the explosive shock front of a Type II supernova passing through the oxygen/neon layer of a 25 \emph{M$_{\odot}$} star. Reaction rates of many (\emph{n,$\gamma$}) reactions and their inverses were increased and decreased by a factor of 3 and the effects were observed. Probing the sensitivity of \emph{p}-nuclei abundances aids in pointing out reactions important to the \emph{p}-process. In turn, this information can be used as a tool to drive experimental research, helping to decrease uncertainties and increase the robustness of \emph{p}-process and other stellar models.