I will discuss equation of state and spin-isospin correlations of hot and dense nucleonic matter found in supernovae and proto-neutron stars. The calculations are done using an ab initio variational many body technique, where the only inputs are the two nucleon and three nucleon interactions in free space. Recently, we showed how a variational theory can be constructed for a system of fermions at finite temperature, which can fully exploit the powerful chain summation techniques developed for theories at zero temperature. I will present results using this method and discuss the consequences for the fate of neutral pion condensation at finite temperature.
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