Neutrino rates in proto-neutron-star matter differ by up to an order of magnitude with the Sky3s Skyrme parametrization versus SLy4, and beta equilibrium is less violated at finite temperature.
Notice that, in the charged-current case, we define τ± = 1 2(τ1 ±iτ 2),(26) whereτ i (i= 1,2,3) are the isospin Pauli matrices
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Charged current neutrino processes in hot nuclear matter with a recent Skyrme parametrization constrained by microscopic calculations
Neutrino rates in proto-neutron-star matter differ by up to an order of magnitude with the Sky3s Skyrme parametrization versus SLy4, and beta equilibrium is less violated at finite temperature.