Influence of the stiffness of the equation of state and in-medium effects on the cooling of compact stars

Abstract

Measurements demonstrate the existence of compact stars with masses in a broad range from 1.2 to 2 $M_{\odot }$. The most massive of these objects might be hybrid stars. To fulfill the constraint $M_{\max }>2M_{\odot }$ with a reserve we exploit the stiff DD2 hadronic equation of state (EoS) without and with excluded volume (DD2vex) correction, which produce maximum neutron star masses of $M_{\max }=2.43M_{\odot }$ and $2.70M_{\odot }$, respectively. We show that the stiffness of the EoS does not preclude an explanation of the whole set of cooling data within "nuclear medium cooling" scenario for compact stars by a variation of the star masses. We select appropriate proton gap profiles from those exploited in the literature and allow for a variation of the effective pion gap controlling the efficiency of the medium modified Urca process. However, we suppress the possibility of pion condensation. In general, the stiffer the EoS the steeper a decrease with density of the effective pion gap is required. Results are compared with previously obtained ones for the HDD EoS for which $M_{\max }=2.06M_{\odot }$. The cooling of the compact star in the supernova remnant Cassiopeia A (Cas A) is explained mainly by an efficient medium modified Urca process. With the DD2vex EoS and using an effective pion gap steeper decreasing with the density and/or a proton gap shifted to smaller densities we are also able to reproduce both a strong decline compatible with ACIS-S data and HRC-S instrument data. The mass of Cas A is estimated as $1.6-1.9M_{\odot }$, above the value $1.5M_{\odot }$, which we have evaluated with the softer HDD equation of state. Different mass choices for the hottest object XMMU J173203.3-344518 are discussed. We make general remarks also on hybrid star cooling and on its dependence on the stiffness of the hadronic EoS.

25 pages, 21 figures, to appear in the EPJA Topical Issue on "Exotic Matter in Neutron Stars"; a strongly abridged version of this work has been presented as eConf C140926 in the Proceedings of the Conference "Compact Stars in the QCD Phase Diagram IV", Prerow, September 26 - 30, 2014; arxiv:1507.04656

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