Abstract
The present status of core-collapse supernova models as well as the role played by neutrons and weak interaction processes are discussed. Special attention is given to the necessary microphysics input data and to possible observational tests. It is demonstrated that certain properties of neutron-rich matter are crucial for the dynamics of supernova explosions including, in particular, the nuclear equation of state. As far as neutrinos are concerned theoretical predictions and expectations are in fairly good agreement with the luminosity and average energy of neutrinos observed from SN 1987A, provided they signaled the formation of a neutron star. In addition, there are indirect ways to constrain the models, such as the optical light curves and nucleosynthesis predictions. They also are discussed.
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