Proto-neutron star convection and the neutrino-driven wind: implications for the r-process

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