  A fully quantitative description of equilibrium and dynamical properties of
hot nuclear matter will be needed for the interpretation of the available and
forthcoming astrophysical data, providing information on the post merger phase
of a neutron star coalescence. We discuss the results of a recently developed
theoretical model,based on a phenomenological nuclear Hamiltonian including
two- and three-nucleon potentials, to study the temperature dependence of
average and single-particle properties of nuclear matter relevant to
astrophysical applications. The potential of the proposed approach for
describing dissipative processes leading to the appearance of bulk viscosity in
neutron star matter is also outlined.
