Cooling of neutron stars with stiff stellar matter
Abstract
Recent evidence for high masses ( 2~ M) pulsars PSR J1614-2230 and PSR J0348-0432 requires neutron star matter to have a stiff equation of state (EoS). The thermal evolution of compact stars (CS) with stiff hadronic EoS necessitates the application of the "nuclear medium cooling" scenario with a selection of appropriate proton gap profiles together with in-medium effects (like pion softening) on cooling mechanisms in order to achieve a satisfactory explanation of all existing observational data for the temperature-age relation of CS. Here we focus on two examples from Grigorian:2016leu for a stiff hadronic EoS without (DD2 EoS) and with (DD2vex) excluded volume correction.
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