Cooling of neutron stars with stiff stellar matter
Abstract
Recent evidence for high masses () 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.
Keywords
Cite
@article{arxiv.1702.01342,
title = {Cooling of neutron stars with stiff stellar matter},
author = {H. Grigorian and D. N. Voskresensky and D. Blaschke},
journal= {arXiv preprint arXiv:1702.01342},
year = {2017}
}
Comments
7 pages, 4 Figures, Contribution to the Proceedings of the International Conference on Critical Point and Onset of Deconfinement (CPOD'2016), Wroclaw, Poland, May 29 - June 5, 2016. arXiv admin note: text overlap with arXiv:1603.02634