Thermal states of neutron stars with a consistent model of interior

Abstract

We model the thermal states of both isolated neutron stars and accreting neutron stars in X-ray transients in quiescence and confront them with observations. We use an equation of state and superfluid baryon gaps, which are consistently calculated. We conclude that the direct Urca process is required to be consistent with low-luminous accreting neutron stars. In addition, proton superfluidity and sufficiently weak neutron superfluidity are necessary to explain the cooling of middle-aged neutron stars and to obtain a realistic distribution of neutron star masses.

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• Thermodynamical Description of Hot, Rapidly Rotating Neutron Stars, Protoneutron Stars, and Neutron Star Merger Remnants
• Limiting magnetic field for minimal deformation of a magnetised neutron star
• Deep crustal heating for realistic compositions of thermonuclear ashes
• Compactness in the Thermal Evolution of Twin Stars
• Thermal evolution of neutron stars in soft X-ray transients with thermodynamically consistent models of the accreted crust
• Nuclear matter at finite temperature and static properties of proto-neutron star
• Cooling of hybrid neutron stars with microscopic equations of state
• Polytropic fits of modern and unified equations of state
• Partially accreted crusts of neutron stars
• Neutron Stars and Gravitational Waves: the Key Role of Nuclear Equation of State
• Nuclear Pairing Gaps and Neutron Star Cooling
• Accurate nuclear symmetry energy at finite temperature within a BHF approach
• Quiescent luminosities of accreting neutron stars with different equation of states
• Neutron star cooling and mass distributions
• Effect of Magnetic Fields on Urca Rates in Neutron Star Mergers
• Cooling of dark neutron stars
• Nonequilibrium thermodynamics of accreted neutron-star crust
• Critical properties of calibrated relativistic mean-field models for the transition to warm, non-homogeneous nuclear matter
• Topology of the Superconducting Heart of Neutron Stars: Effects of Microphysics and Gravitational-Wave Signatures
• A solution to the tension of burning on neutron stars and nuclear physics