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

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arxiv 2304.07836 v2 pith:C5VQWP2R submitted 2023-04-16 nucl-th astro-ph.HEhep-ph

Mark G. Alford , Liam Brodie , Alexander Haber , Ingo Tews This is my paper · ORCID
classification nucl-thastro-ph.HEhep-ph
keywords matterneutronnuclearstartheorychargechiralcompose
verification ladder T0 review T1 audit T2 compute T3 formal

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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.

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Cited by 3 Pith papers

Reviewed papers in the Pith corpus that reference this work. Sorted by Pith novelty score. Full citation record

  1. Binary neutron stars in the next-generation era: Multi-messenger detection prospects and constraints on the equation of state, mass distribution, and cosmology

    astro-ph.HE 2026-07 conditional novelty 6.0 of 10

    With ET (and ET+CE), mock multi-messenger BNS catalogues yield ~40–500 EM counterparts per year and, under ideal recovery, constrain R1.4 to ~0.2 km and H0 to ~1 km s−1 Mpc−1.

  2. Determining the minimal mass of a proto-neutron star with chirally constrained nuclear equations of state

    nucl-th 2024-11 conditional novelty 6.0 of 10

    For chirally constrained nuclear equations of state, the minimal proto-neutron star mass is about 0.62 solar masses with trapped neutrinos (YL=0.4, s=1) and about 0.22 solar masses after deleptonization (s=2).

  3. Transport properties in binary neutron star mergers: Effect of magnetic field

    nucl-th 2026-08 conditional novelty 5.0 of 10

    Magnetic fields up to 5e17 G increase charged-current neutrino and antineutrino opacities in neutron star merger matter by up to two orders of magnitude at low temperature, shrinking neutrino mean free paths.

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