Hot and dense neutron-rich matter in supernovae and neutron star mergers

Abstract:  Recently, the first confirmed observation of a binary neutron star merger through its gravitational wave (GW170817) and associated electromagnetic emissions has opened a new window into our understanding of ultra-dense matter. Supercomputer simulations of these events relies on detailed knowledge of the equation of state, transport and linear response properties of hot and dense neutron-rich matter. In this talk I will describe recent progress in modeling the strong interaction physics of neutron stars and supernovae based on the low-energy realization of QCD, chiral effective field theory. I will demonstrate how our present understanding of nuclear physics is already consistent with the gravitational wave signal from GW170817 but that there are strong prospects for stronger constraints from upcoming observational campaigns of neutron stars.