  The neutrino-driven wind from proto-neutron stars is a proposed site for
r-process nucleosynthesis, although most previous work has found that a wind
heated only by neutrinos cannot produce the third r-process peak. However,
several groups have noted that introducing a secondary heating source within
the wind can change the hydrodynamic conditions sufficiently for a strong
r-process to proceed. One possible secondary heating source is gravito-acoustic
waves, generated by convection inside the proto-neutron star. As these waves
propagate into the wind, they can both accelerate the wind and shock and
deposit energy into the wind. Additionally, the acceleration of the wind by
these waves can reduce the total number of neutrino captures and thereby reduce
the final electron fraction of the wind. In neutron rich conditions, all of
these effects can make conditions more favorable for r-process nucleosynthesis.
Here, we present a systematic investigation of the impact of these
convection-generated gravito-acoustic waves within the wind on potential
nucleosynthesis. We find that wave effects in the wind can generate conditions
favorable for a strong r-process, even when the energy flux in the waves is a
factor of $10^{-4}$ smaller than the total neutrino energy flux and the wind is
marginally neutron-rich. Nevertheless, this depends strongly on the radius at
which the wave become non-linear and form shocks. We also find that both
entropy production after shock formation and the acceleration of the wind due
to stresses produced by the waves prior to shock formation impact the structure
and nucleosynthesis of these waves.
