Unraveling the global behavior of equation of state by explicit finite nuclei constraints

TL;DR

This paper derives a broad range of equations of state (EOSs) for nuclear matter by explicitly incorporating finite nuclei constraints, heavy-ion collision data, and neutron star observations, revealing distinct global behaviors.

Contribution

It introduces an explicit method for applying finite nuclei constraints to EOS determination, leading to different EOS characteristics compared to traditional implicit approaches.

Findings

Explicit constraints produce softer EOSs at low densities.

Resulting EOSs become stiffer at high densities to support neutron star masses.

Quantitative comparison shows significant differences in neutron star property distributions.

Abstract

We obtain posterior distribution of equations of state (EOSs) across a broad range of density by imposing explicitly the constraints from precisely measured fundamental properties of finite nuclei, in combination with the experimental data from heavy-ion collisions and the astrophysical observations of radius, tidal deformability and minimum-maximum mass of neutron stars. The acquired EOSs exhibit a distinct global behavior compared to those usually obtained by imposing the finite nuclei constraints implicitly through empirical values of selected key parameters describing symmetric nuclear matter and symmetry energy in the vicinity of the saturation density. The explicit treatment of finite nuclei constraints yields softer EOSs at low densities which eventually become stiffer to meet the maximum mass criteria. The Kullback-Leibler divergence has been used to perform a quantitative comparison of the distributions of neutron star properties resulting from the EOSs obtained from implicit and explicit finite nuclei constraints.