  Neutrino-driven winds that follow core-collapse supernovae are an exciting
astrophysical site for the production of heavy elements. Although
hydrodynamical simulations show that the conditions in the wind are not extreme
enough for a r-process up to uranium, neutrino-driven winds may be the
astrophysical site where lighter heavy elements between Sr an Ag are produced,
either by the weak r-process or by the $\nu \!p$-process. However, it is still
not clear if the conditions in the wind are slightly neutron-rich or
proton-rich. Therefore, we investigate the nucleosynthesis in the wind for
neutron- and proton-rich conditions and systematically explore the impact of
wind parameters on abundances. Here we focus on molybdenum that has raised
attention because several astrophysical scenarios failed to reproduce the solar
system (SoS) abundance ratio of $^{92}\mathrm{Mo}$ and $^{94}\mathrm{Mo}$.
Moreover, available data of SiC X grains exhibit different isotopic ratios of
$^{95}\mathrm{Mo}$ and $^{97}\mathrm{Mo}$ than in the SoS. We have investigated
if neutrino-driven winds can reproduce the SoS
$Y(^{92}\mathrm{Mo})/Y(^{94}\mathrm{Mo})$ and can explain the origin of the
$Y(^{95}\mathrm{Mo})/Y(^{97}\mathrm{Mo})$ found in SiC X.
