Abstract
Just after the phase transition from hadronic to quark matter in neutron stars, weak interactions drive quark matter to thermal and chemical equilibrium. We calculate the reaction rate and the neutrino emissivity for all the relevant weak interaction processes in hot and dense quark matter and solve the Boltzmann equation in order to describe the time evolution of the system. We find that the neutrino emissivity per baryon is very large, leading to an energy release per baryon of 10–60 MeV in the form of neutrinos.
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