The most detailed calculations of the p-process call for its development in the O/Ne layers of Type II supernovae. In spite of their overall success in reproducing the solar system content of p-nuclides, they suggest a significant underproduction of the light Mo and Ru isotopes. On grounds of a model for the explosion of a 25 M-circle dot star with solar metallicity, we demonstrate that this failure might just be related to the uncertainties left in the rate of the Ne-22(alpha ,n) Mg-25 neutron producing reaction. The latter indeed has a direct impact on the distribution of the s-process seeds for the p-process. [References: 15]
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