Thermal effects on nuclear matter properties
arXiv:2208.03131 · doi:10.1103/PhysRevD.106.103020
Abstract
A quantitative description of the properties of hot nuclear matter will be needed for the interpretation of the available and forthcoming astrophysical data, providing information on the post merger phase of a neutron star coalescence. We have employed a recently developed theoretical model, based on a phenomenological nuclear Hamiltonian including two- and three-nucleon potentials, to study the temperature dependence of average and single-particle properties of nuclear matter relevant to astrophysical applications. The possibility to represent the results of microscopic calculations using simple and yet physically motivated parametrisations of thermal effects, suitable for use in numerical simulations of astrophysical processes, is also discussed.
References in corpus (41)
- An accurate nucleon-nucleon potential with charge-independence breaking
- The equation of state for nucleon matter and neutron star structure
- Quantum Monte Carlo Calculations of Nuclei
- Composition and Structure of Protoneutron Stars
- Evolution of Protoneutron Stars
- Binary neutron-star mergers: a review of Einstein's richest laboratory
- Constraining the speed of sound inside neutron stars with chiral effective field theory interactions and observations
- Constraining the neutron-proton effective mass splitting using empirical constraints on the density dependence of nuclear symmetry energy around normal density
- Evolution of Nuclear Spectra with Nuclear Forces
- Binary Neutron Star Mergers: Dependence on the Nuclear Equation of State
- Spin-Isospin Structure and Pion Condensation in Nucleon Matter
- Relativistic neutron star merger simulations with non-zero temperature equations of state I. Variation of binary parameters and equation of state
- Testing Approximations of Thermal Effects in Neutron Star Merger Simulations
- On the importance of viscous dissipation and heat conduction in binary neutron-star mergers
- Gravitational waves and mass ejecta from binary neutron star mergers: Effect of the mass-ratio
- Thermodynamics conditions of matter in neutron star mergers
- Numerical Relativity Simulations of the Neutron Star Merger GW170817: Long-Term Remnant Evolutions, Winds, Remnant Disks, and Nucleosynthesis
- Accretion-induced prompt black hole formation in asymmetric neutron star mergers, dynamical ejecta and kilonova signals
- The Influence of Thermal Pressure on Equilibrium Models of Hypermassive Neutron Star Merger Remnants
- Gravitational waves and mass ejecta from binary neutron star mergers: Effect of the stars' rotation
- Beta equilibrium in neutron star mergers
- Nuclear thermodynamics from chiral low-momentum interactions
- General Relativistic Magnetohydrodynamic Simulations of Binary Neutron Star Mergers with the APR4 Equation of State
- Evolution of a proto-neutron star with a nuclear many-body equation of state: Neutrino luminosity and gravitational wave frequencies
- constraints on thermal effects of the nuclear equation of state
- Nuclear and neutron matter -matrix calculations with Ch-EFT potential including effects of three-nucleon interaction
- Finite-temperature extension for cold neutron star equations of state
- Shear viscosity of neutron matter from realistic nucleon-nucleon interactions
- The maximum and minimum mass of protoneutron stars in the Brueckner theory
- Thermodynamics conditions of matter in the neutrino decoupling region during neutron star mergers
- Hybrid equation of state approach in binary neutron-star merger simulations
- Neutron matter at finite temperature based on chiral effective field theory interactions
- Microscopic equation of state of hot nuclear matter for numerical relativity simulations
- Neutrino emission from binary neutron star mergers: characterizing light curves and mean energies
- Hot neutron stars with microscopic equations of state
- Bulk viscosity from Urca processes: matter in the neutrino-trapped regime
- Benchmark calculations of infinite neutron matter with realistic two- and three-nucleon potentials
- Axisymmetric models for neutron star merger remnants with realistic thermal and rotational profiles
- Weak response of cold symmetric nuclear matter at three-body cluster level
- Binary neutron star merger simulations with hot microscopic equations of state
- Modeling Neutron Star Matter in the Age of Multimessenger Astrophysics