Neutron star cooling with microscopic equations of state

Abstract

We model neutron star cooling with several microscopic nuclear equations of state based on different nucleon-nucleon interactions and three-body forces, and compatible with the recent GW170817 neutron star merger event. They all feature strong direct Urca processes. We find that all models are able to describe well the current set of cooling data for isolated neutron stars, provided that large and extended proton 1S0 gaps and no neutron 3PF2 gaps are active in the stellar matter. We then analyze the neutron star mass distributions predicted by the different models and single out the preferred ones.

arXiv comment8 pages, 5 figures

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• Neutron Stars and the Nuclear Equation of State
• Thermal luminosities of cooling neutron stars
• Proto-neutron stars with heavy baryons and universal relations
• Beta equilibrium under neutron star merger conditions
• Thermal evolution and quiescent emission of transiently accreting neutron stars
• Hot neutron stars with microscopic equations of state
• Nucleon effective mass in hot dense matter
• Efficient estimation method for time evolution of proto-neutron star mass and radius from supernova neutrino signal
• Microscopic nuclear equation of state at finite temperature and stellar stability
• Cooling of hybrid neutron stars with microscopic equations of state
• Nuclear Pairing Gaps and Neutron Star Cooling
• Accurate nuclear symmetry energy at finite temperature within a BHF approach
• Neutron star cooling and mass distributions
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• Cooling of dark neutron stars
• Binary Neutron Star (BNS) merger: What we learned from relativistic ejecta of GW/GRB~170817A