Influence of neutrino-matter reaction rates in core-collapse supernovae and proto-neutron star cooling simulationsHYBRID

The complete modeling of core-collapse supernovae and proto-neutron star cooling involves many fields of physics including, among others, general-relativistic magneto-hydrodynamics, neutrino transport or properties of ultra dense matter. Although a full numerical model including state-of-the art approaches to each of the aforementioned fields is still beyond the reach of current computing facilities, several teams are now performing three-dimensional general-relativistic core-collapse simulations, including realistic equation of state and approximate neutrino transport. In this presentation, after an introduction to the subject and a description of our numerical models, I will give some results from our group where we have adopted a different approach, namely the testing of the influence of various improvements in the computations of neutrino reaction rates (electron-capture, neutrino-nucleon interactions, etc) and properties of dense matter, within a simplified numerical setting.