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We perform simulations of the Kelvin-Helmholtz cooling phase of proto-neutronstars with a new numerical code in spherical symmetry and using thequasi-static approximation. We use for the first time the full set ofcharged-current neutrino-nucleon reactions, including neutron decay andmodified Urca processes, together with the energy-dependent numericalrepresentation for the inclusion of nuclear correlations with random-phaseapproximation. Moreover, convective motions are taken into account within themixing-length theory. As we vary the assumptions for computing neutrino-nucleonreaction rates, we show that the dominant effect on the cooling timescale,neutrino signal and composition of the neutrino-driven wind comes from theinclusion of convective motion. Computation of nuclear correlations within therandom phase approximation, as compared to mean field approach, has arelatively small impact.

Proto-neutron star evolution with improved charged-current neutrino-nucleon interactions