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Our understanding of the core-collapse supernova explosion mechanism isincomplete. While the favoured scenario is delayed revival of the stalled shockby neutrino heating, it is difficult to reliably compute explosion outcomes andenergies, which depend sensitively on the complex radiation hydrodynamics ofthe post-shock region. The dynamics of the (non-)explosion depend sensitivelyon how energy is transported from inside and near the proto-neutron star (PNS)to material just behind the supernova shock. Although most of the PNS energy islost in the form of neutrinos, hydrodynamic and hydromagnetic waves can alsocarry energy from the PNS to the shock. We show that gravity waves excited bycore PNS convection can couple with outgoing acoustic waves that present anappreciable source of energy and pressure in the post-shock region. Usingone-dimensional simulations, we estimate the gravity wave energy flux excitedby PNS convection and the fraction of this energy transmitted upward to thepost-shock region as acoustic waves. We find wave energy fluxes near$10^{51}\,\mathrm{erg}\,\mathrm{s}^{-1}$ are likely to persist for$\sim1\,\mathrm{s}$ post-bounce. The wave pressure on the shock may exceed$10\%$ of the thermal pressure, potentially contributing to shock revival and,subsequently, a successful and energetic explosion. We also discuss how futuresimulations can better capture the effects of waves, and more accuratelyquantify wave heating rates.

Wave heating from proto-neutron star convection and the core-collapse supernova explosion mechanism