Neutron star cooling and mass distributions
arXiv:2403.02222 · doi:10.1103/PhysRevD.109.123018
Abstract
We study the cooling of isolated neutron stars, employing different nuclear equations of state with or without active direct Urca process, and investigate the interplay with the nuclear pairing gaps. We find that a consistent description of all current cooling data requires fast direct Urca cooling and reasonable proton 1S0 gaps, but no neutron 3P2 pairing. We then deduce the neutron star mass distributions compatible with the cooling analysis and compare with current theoretical models. Reduced 1S0 gaps and unimodal mass distributions are preferred by the analysis. The importance of statistical and systematic errors is also investigated.
14 pages, 10 figures, 2 tables, Published in Phys. Rev. D
References in corpus (19)
- GW170817: Observation of Gravitational Waves from a Binary Neutron Star Inspiral
- Shapiro delay measurement of a two solar mass neutron star
- PSR J0030+0451 Mass and Radius from NICER Data and Implications for the Properties of Neutron Star Matter
- A NICER View of PSR J0030+0451: Millisecond Pulsar Parameter Estimation
- Neutron Star Observations: Prognosis for Equation of State Constraints
- PSR J0952-0607: The Fastest and Heaviest Known Galactic Neutron Star
- GW170817: Joint Constraint on the Neutron Star Equation of State from Multimessenger Observations
- Thermal luminosities of cooling neutron stars
- Nucleon effective masses within the Brueckner-Hartree-Fock theory: Impact on stellar neutrino emission
- Statistical theory of thermal evolution of neutron stars
- Statistical theory of thermal evolution of neutron stars - II. Limitations on direct Urca threshold
- Pairing in neutron matter: New uncertainty estimates and three-body forces
- Nuclear pairing from microscopic forces: singlet channels and higher-partial waves
- Thermal states of neutron stars with a consistent model of interior
- Dark matter effects on the properties of neutron stars: optical radii
- Microscopic nuclear equation of state at finite temperature and stellar stability
- Three-nucleon forces and superfluidity in neutron matter
- Modified Urca neutrino emissivity at finite temperature
- Hybrid cooling of the Cassiopeia A neutron star