  Core-collapse supernovae are the first polluters of heavy elements in the
galactic history. As such, it is important to study the nuclear compositions of
their ejecta, and understand their dependence on the progenitor structure
(e.g., mass, compactness, metallicity). Here, we present a detailed
nucleosynthesis study based on two long-term, two-dimensional core-collapse
supernova simulations of a 11.2 M$_{\odot}$ and a 17.0 M$_{\odot}$ star. We
find that in both models nuclei well beyond the iron group (up to $Z \approx
44$) can be produced, and discuss in detail also the nucleosynthesis of the
p-nuclei $^{92,94}$Mo and $^{96,98}$Ru. While we observe the production of
$^{92}$Mo and $^{94}$Mo in slightly neutron-rich conditions in both
simulations, $^{96,98}$Ru can only be produced efficiently via the
$\nu$p-process. Furthermore, the production of Ru in the $\nu$p-process heavily
depends on the presence of very proton-rich material in the ejecta. This
disentanglement of production mechanisms has interesting consequences when
comparing to the abundance ratios between these isotopes in the solar system
and in presolar grains.
