Compression modulus and symmetry energy of nuclear matter with KIDS density functional

TL;DR

This paper uses the KIDS density functional theory to constrain the nuclear matter equation of state by combining nuclear data and neutron star observations, reducing uncertainties and analyzing effects on nuclear properties.

Contribution

It introduces a method to constrain the equation of state parameters using combined nuclear and astrophysical data within the KIDS density functional framework.

Findings

Uncertainty in the equation of state parameters is significantly reduced.

The constrained parameters accurately reproduce properties of spherical magic nuclei.

Neutron drip lines depend on the nuclear symmetry energy uncertainty.

Abstract

Equation of state of dense nuclear matter is explored in the KIDS density functional theory. Parameters of the equation of state which are coefficients of the energy density expanded in powers of $(\rho - \rho_0)/3\rho_0$ where $\rho$ is the nuclear matter density and $\rho_0$ is its density at saturation are constrained by using both nuclear data and the mass-radius relation of the neutron star determined from the modern astronomy. We find that the combination of both data can reduce the uncertainty in the equation of state parameters significantly. We confirm that the newly constrained parameters reproduce the basic properties of spherical magic nuclei with high accuracy. Neutron drip lines, on the other hand, show non-negligible dependence on the uncertainty of the nuclear symmetry energy.