Hot neutron stars and their equation of state
arXiv:2112.05323 · doi:10.1103/PhysRevC.104.065806
Abstract
A set of microscopic, covariant density-functional, and non-relativistic Skyrme-type equations of state is employed to study the structure of purely nucleonic neutron stars at finite temperature. After examining the agreement with presently available astrophysical observational constraints, we find that the magnitude of thermal effects depends on the nucleon effective mass as well as on the stiffness of the cold equation of state. We evidence a fairly small but model-dependent effect of finite temperature on stellar stability that is correlated with the relative thermal pressure inside the star.
10 pages, 8 figures
References in corpus (28)
- GW170817: Observation of Gravitational Waves from a Binary Neutron Star Inspiral
- 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
- A NICER View of the Massive Pulsar PSR J0740+6620 Informed by Radio Timing and XMM-Newton Spectroscopy
- Constraining the Maximum Mass of Neutron Stars From Multi-Messenger Observations of GW170817
- Neutron-Rich Nuclei in Heaven and Earth
- Modeling GW170817 based on numerical relativity and its implications
- Relativistic effective interaction for nuclei, giant resonances, and neutron stars
- Neutron Stars and the Nuclear Equation of State
- Nuclear equation of state for core-collapse supernova simulations with realistic nuclear forces
- A lower bound on the maximum mass if the secondary in GW190814 was once a rapidly spinning neutron star
- Tables of Hyperonic Matter Equation of State for Core-Collapse Supernovae
- A New Open-Source Nuclear Equation of State Framework based on the Liquid-Drop Model with Skyrme Interaction
- Equation of State for Nucleonic and Hyperonic Neutron Stars with Mass and Radius Constraints
- A new temperature dependent hyperonic equation of state: application to rotating neutron star models and I-Q-relations
- The Equation of State for the Nucleonic and Hyperonic Core of Neutron Stars
- The Vlasov formalism for extended relativistic mean field models: the crust-core transition and the stellar matter equation of state
- Nucleon effective masses within the Brueckner-Hartree-Fock theory: Impact on stellar neutrino emission
- Importance of cooling in triggering the collapse of hypermassive neutron stars
- Finite-temperature extension for cold neutron star equations of state
- Effects of the symmetry energy on properties of neutron star crusts near the neutron drip density
- Maximum mass of compact stars from gravitational wave events with finite-temperature equations of state
- Hybrid equation of state approach in binary neutron-star merger simulations
- EoS for hot neutron stars
- Variational Calculation for the Equation of State of Nuclear Matter at Finite Temperatures
- Protoneutron stars in the Brueckner-Hartree-Fock approach and finite-temperature kaon condensation
- The equation of state and radial oscillations of neutron stars
- Binary neutron star merger simulations with hot microscopic equations of state
Cited by in corpus (7)
- Equations of state for hot neutron stars -- II. The role of exotic particle degrees of freedom
- Universal relations for rapidly rotating cold and hot hybrid star
- Microscopic nuclear equation of state at finite temperature and stellar stability
- Frequencies of - and -oscillation modes in cold and hot compact stars
- Thermodynamics of Hot Neutron Stars and Universal Relations
- Investigating Possible Existence of Hyper-Heavy Nuclei in Neutron Star Environment
- New ab initio constrained extended Skyrme equations of state for simulations of neutron stars, supernovae and binary mergers: II. Thermal response in the suprasaturation density domain