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arXiv · 1702.01342

Cooling of neutron stars with stiff stellar matter

H. Grigorian·D. N. Voskresensky·D. Blaschke
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Abstract

Recent evidence for high masses ($\sim 2~ M_\odot$) 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 \cite{Grigorian:2016leu} for a stiff hadronic EoS without (DD2 EoS) and with (DD2vex) excluded volume correction.

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H. Grigorian, D. N. Voskresensky, D. Blaschke. 2017-02-04. Cooling of neutron stars with stiff stellar matter. https://doi.org/10.5506/aphyspolbsupp.10.819

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