  We present a new nucleosynthesis process that may take place on neutron-rich
ejecta experiencing an intensive neutrino flux. The nucleosynthesis proceeds
similarly to the standard $r$-process, a sequence of neutron-captures and
beta-decays, however with charged-current neutrino absorption reactions on
nuclei operating much faster than beta-decays. Once neutron capture reactions
freeze-out the produced $r$-process neutron-rich nuclei undergo a fast
conversion of neutrons into protons and are pushed even beyond the
$\beta$-stability line producing the neutron-deficient $p$-nuclei. This
scenario, which we denote as the $\nu r$-process, provides an alternative
channel for the production of $p$-nuclei and the short-lived nucleus $^{92}$Nb.
We discuss the necessary conditions posed on the astrophysical site for the
$\nu r$-process to be realized in nature. While these conditions are not
fulfilled by current neutrino-hydrodynamic models of $r$-process sites, future
models, including more complex physics and a larger variety of outflow
conditions, may achieve the necessary conditions in some regions of the ejecta.
