Abstract. We study the sensitivity of the νp-process abundance pattern to (n,p), (p,γ), and (n,γ) rates for nuclei between Ni and Sn. We illustrate our findings for two different initial electron fractions and a representative trajectory. We discuss how these rates influence the abundance pattern and the nuclear flow.

In understanding the origin of the heavy elements, the "light heavy elements" pose a particular challenge: The two neutron-capture processes, r-process and s-process, cannot explain the abundances patterns seen in very old galactic halo stars. A proposed solution to this problem is the νp-process, which takes place in the strong neutrino-driven winds of core-collapse supernovae. In the νp-process, a sequence of (n,p) and (p,γ) reactions allows for the synthesis of elements with atomic numbers A > 64, which includes Sr, Y, Zr, and others possibly up to Sn. The relevant reaction rates are all based on statistical model predictions and carry some uncertainty. Here, the sensitivity of the final νp-process abundance pattern on modifications of (n,p), (p,γ), and (n,γ) reactions are characterized. Only few reactions affect the final abundance pattern and hence warrant a more detailed study of the reaction rate.