Speaker
Description
We present one of the first results obtained with NSCool 2D Rot, a major upgrade of 1D neutron stars thermal evolution code NSCool by D. Page. Our new code allows to model thermal evolution of axisymmetric rotating neutron stars with arbitrary rotation frequencies up to the mass shedding limit in full general relativity. As an application, we address the question of cooling of rapidly rotating isolated neutron stars. We study the impact of equation of state (EOS) on the cooling by considering different EOSs of the core and crust. Simulation results show complex time-dependent dynamics of temperature distribution in the crust of the star. Nevertheless, we demonstrate that most of that complexity can be explained by formation of a ``heat blob'' in the crust and by timescales of heat diffusion through the crust.