Simulation of neutrino transport by large-scale convective instability in a proto-neutron star

Neutrino transfer via convective flow to the surface of a proto-neutron sta r is numerically simulated. The evolution of the neutrino distribution in a heated region rising from the center of the proto-neutron star to its surf ace is simulated using a kinetic equation with a Uehling-Uhlenbeck collisio n integral in a uniform, isotropic approximation. The composition of the ma tter in the region under consideration changes due to the "burning" of elec trons and protons by beta processes. The simulation results enable the esti mation of the characteristic time required for the rising medium to become optically thin to neutrinos and the characteristic spectrum of the neutrino s that are emitted. (C) 2001 MAIK "Nauka/Interperiodica".