Tabulated Neutron Star Equations of State Modeled within the Chiral Mean Field Model
V. Dexheimer
TL;DR
This paper reviews the chiral mean field (CMF) model's application to neutron star physics, presenting tabulated equations of state and particle populations for various astrophysical environments.
Contribution
It introduces a comprehensive set of CMF-based equations of state and particle data tailored for different neutron star and supernova conditions.
Findings
Developed EOS tables consistent with physical constraints
Applied CMF model to diverse astrophysical scenarios
Enhanced understanding of matter in extreme environments
Abstract
In this special issue article, I review some of the accomplishments of the chiral mean field (CMF) model, which contains nucleon, hyperon, and quark degrees of freedom, and its applications to proto-neutron and neutron stars. I also present a set of equation of state and particle population tables built using the CMF model subject to physical constraints necessary to reproduce different environments, such as those present in cold neutron stars, core-collapse supernova explosions and different stages of compact star mergers.
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