  Recent studies of the neutrino-driven wind from proto-neutron stars have
indicated that the wind is likely proton-rich for much of its lifetime, and the
high flux of neutrinos can induce $\nu$p-process nucleosynthesis allowing for
the formation of heavy elements. It has also been shown that gravito-acoustic
waves, generated by convection within the proto-neutron star, can significantly
alter the dynamics and nucleosynthesis in the wind. Therefore, we present a
study of the effects of convection-driven waves on the nucleosynthesis in
proton-rich neutrino-driven winds, focusing on the $\nu$p-process. We find that
wave effects can strongly impact $\nu$p-process nucleosynthesis even at wave
luminosities a factor of $10^{-5}$ smaller than the total neutrino luminosity.
The momentum flux of the waves accelerates the wind, reducing the net neutrino
heating and the persistent neutron abundance created by p($\bar{\nu}_e,e^+$),
which impedes $\nu$p-process nucleosynthesis. However, this effect is generally
counteracted by the effects of waves on seed nucleus formation, as the
acceleration of the wind and the heating that occurs as these waves shock both
favor a more $\alpha$-rich environment with very little heavy seed-nucleus
formation. Overall, higher wave luminosities correlate (albeit
non-monotonically) with heavier element $\nu$p-processing, up to $A\approx 200$
in some cases. At very high wave luminosities ($\gtrsim 10^{-3}L_\nu$), early
shock heating by the waves disrupts $\alpha$ recombination, and drives a
suppressed, fast-outflow r-process proceeding up to $A\approx 200$. This occurs
despite an assumed neutrino spectrum that predicts a proton-rich wind with
equilibrium $Y_e=0.6$.
