Incompressibility and Symmetry Energy of Neutron Star

TL;DR

This paper develops a systematic method to accurately determine key structural and compositional properties of neutron stars, such as incompressibility and symmetry energy, using relativistic energy density functionals and the coherent density fluctuation model.

Contribution

It introduces a novel analytical approach to evaluate neutron star properties based on polynomial fits of saturation curves and relativistic mean-field models.

Findings

NL3 set yields higher property magnitudes due to stiffer equation of state.

The method provides consistent numerical estimates for neutron star properties.

Incompressibility and symmetry energy are quantified for different parameter sets.

Abstract

We trace a systematic and consistent method to precisely numerate the magnitude range for various structural and isospin compositional properties of the neutron star. Incompressibility, symmetry energy, slope parameter and curvature of a neutron star are investigated using the relativistic energy density functional within the framework of coherent density fluctuation model. The analytical expression for the energy density functional of the neutron star matter is motivated from the Br$\ddot{u}$ckner functional and acquired by the polynomial fitting of the saturation curves for three different relativistic mean-field parameter sets (NL3, G3 and IU-FSU). The modified functional is folded with the neutron star's density-dependent weight function to calculate the numerical values for incompressibility and symmetry energy using the coherent density fluctuation model. NL3 parameter set, being the stiffest equation of state, endue us with a higher magnitude of all the properties compared to the other two parameter sets.