Neutron star evolutionary sequences

We present detailed numerical calculations of the evolution of neutron stars that are cooling through the range of central temperatures from about 10/sup 10/ to 10/sup 7/ K. The calculations are solutions of the full set of central relativistic equations that describe the evolution of a spherical star. We have employed the best current expressions for transport processes and neutrino emission rates and have been particularly careful in our treatment of the thermal properties of neutron star matter. Specifically, we have included the effects of nucleon superfluidity in the inner crust and core, and we have constructed models with and without a pion condensate at high densities. We have also included a variety of thermal contributions due to nuclei in the inner crust, and in some sequences we have followed the crystallization of the crust in order to investigate the consequences of this process for the evolution.