Simulation of Neutrino Transport by Large-Scale Convective Instability in a Proto-Neutron Star

Details Simulation of Neutrino Transport by Large-Scale Convective Instability in a Proto-Neutron Star Simulation of Neutrino Transport by Large-Scale Convective Instability in a Proto-Neutron Star

Mar 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001arep...45..241s&link_type=abstract

Astronomy Reports, Volume 45, Issue 3, March 2001, pp.241-247

Astronomy and Astrophysics

Astronomy

3

Scientific paper

Neutrino transfer via convective flow to the surface of a proto-neutron star is numerically simulated. The evolution of the neutrino distribution in a heated region rising from the center of the proto-neutron star to its surface is simulated using a kinetic equation with a Uehling-Uhlenbeck collision integral in a uniform, isotropic approximation. The composition of the matter in the region under consideration changes due to the “burning” of electrons and protons by beta processes. The simulation results enable the estimation of the characteristic time required for the rising medium to become optically thin to neutrinos and the characteristic spectrum of the neutrinos that are emitted.

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