Tabulated Equations of State From Models Informed by Chiral Effective Field Theory

Abstract

We construct four equation of state (EoS) tables, tabulated over a range of temperatures, densities, and charge fractions, relevant for neutron star applications such as simulations of neutron star mergers. The EoS are computed from a relativistic mean-field theory constrained by the pure neutron matter EoS from chiral effective field theory, inferred properties of isospin-symmetric nuclear matter, and astrophysical observations of neutron star structure. To model nuclear matter at low densities, we attach an EoS that models inhomogeneous nuclear matter at arbitrary temperatures and charge fractions. The four EoS tables we develop are available from the CompOSE EoS repository compose.obspm.fr/eos/297 and gitlab.com/ahaber/qmc-rmf-tables.

8 pages, 3 figures v2: version published in Phys. Scr. 98, added finite T chiral EFT comparison

References in corpus (6)

• 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
• Chiral effective field theory and nuclear forces
• Relativistic effective interaction for nuclei, giant resonances, and neutron stars
• Relativistic mean-field theories for neutron-star physics based on chiral effective field theory
• Bulk Viscosity of Relativistic $npe\mu$ Matter in Neutron-Star Mergers

Cited by in corpus (8)

• A Bayesian mixture model approach to quantifying the empirical nuclear saturation point
• Investigating the role of nuclear parameters on oscillation modes in hot Neutron Stars
• Nonparametric extensions of nuclear equations of state: probing the breakdown scale of relativistic mean-field theory
• Effect of Magnetic Fields on Urca Rates in Neutron Star Mergers
• Determining the minimal mass of a proto-neutron star with chirally constrained nuclear equations of state
• Suppression of composition $g$-modes in chemically-equilibrating warm neutron stars
• Thermal and Magnetic effects on Bulk Viscosity in Binary Neutron Star Mergers
• Parity-doubled nucleons can rapidly cool neutron stars