Influence of effective nucleon mass on equation of state for supernova simulations and neutron stars

Abstract

We investigate the influence of the effective nucleon mass on the equation of state (EOS), which is constructed for simulations of core-collapse supernovae and binary neutron star mergers, within the relativistic mean-field (RMF) framework. The study introduces a new RMF parameter set, TM1m, which is a modification of the TM1e model with an adjusted effective mass, maintaining the saturation properties of nuclear matter. The TM1m model, with a larger effective mass ratio ($M^{\ast }/M\sim 0.8$) compared to the TM1e model ($M^{\ast }/M\sim 0.63$), is employed to construct a new EOS table, EOS5. This EOS table is designed to offer insights into the influence of the effective nucleon mass on the EOS within a relativistic framework, particularly above the saturation density. The results of EOS5 are compared with those obtained from other models, including both relativistic and nonrelativistic approaches. The properties of cold neutron stars, calculated using the TM1m model, are compatible with the existence of a $2M_{\odot }$ pulsar and the latest constraints on the tidal deformability and radii of a canonical $1.4M_{\odot }$ neutron star, derived from astrophysical observations.

11 pages, 11 figures, 2 tables

References in corpus (21)

• GW170817: Observation of Gravitational Waves from a Binary Neutron Star Inspiral
• A Massive Pulsar in a Compact Relativistic Binary
• 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
• Relativistic Mean-Field Hadronic Models under Nuclear Matter Constraints
• Relativistic effective interaction for nuclei, giant resonances, and neutron stars
• Building relativistic mean field models for finite nuclei and neutron stars
• Nuclear equation of state for core-collapse supernova simulations with realistic nuclear forces
• The symmetry energy at subnuclear densities and nuclei in neutron star crusts
• Hadron-quark mixed phase in hyperon stars
• 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
• A Second Relativistic Mean Field and Virial Equation of State for Astrophysical Simulations
• A new equation of state for core-collapse supernovae based on realistic nuclear forces and including a full nuclear ensemble
• Effects of the symmetry energy on properties of neutron star crusts near the neutron drip density
• Comparing treatments of weak reactions with nuclei in simulations of core-collapse supernovae
• Thermal evolution of relativistic hyperonic compact stars with calibrated equations of state
• Cooling timescale for protoneutron stars and properties of nuclear matter: Effective mass and symmetry energy at high densities
• Effects of nuclear symmetry energy and equation of state on neutron star properties
• Constraints on Nuclear Saturation Properties from Terrestrial Experiments and Astrophysical Observations of Neutron Stars
• The Hadron-Quark Crossover in Neutron Star within Gaussian Process Regression Method

Cited by in corpus (6)

• Influence of the effective mass on the properties of nuclear matter at finite density and temperature
• Equation of state for hyperonic neutron-star matter in SU(3) flavor symmetry
• $f$ and $p$ mode oscillation of proto-neutron stars with systematic variation of the nucleon effective mass
• Effects of a Brueckner-Hartree-Fock-corrected effective mass on speed of sound, conformality, and observables of dark matter-admixed neutron stars
• Kaon-meson coupling from SU(3) flavour symmetry and application to antikaon condensed dense matter in neutron star
• Nuclear Matter and Finite Nuclei: Relativistic Thomas-Fermi Approximation Versus Relativistic Mean-Field Approach