Constraining the density dependence of symmetry energy using mean field models

TL;DR

This paper investigates how the density dependence of nuclear symmetry energy can be constrained using mean field models, focusing on empirical parameters J, L, and K_sym relevant to nuclear and astrophysical systems.

Contribution

It provides a systematic analysis of the density dependence of symmetry energy using mean field models and explores how to better constrain the parameters L and K_sym from experimental data.

Findings

J is well constrained by binding energy data

L and K_sym remain uncertain and require further experimental constraints

Mean field models help relate empirical parameters to observable quantities

Abstract

The nuclear symmetry energy characterizes the variation of the binding energy as the neutron to proton ratio of nuclear systems (e.g. finite nucleus, neutron star etc.) is varied. The densities associated to these nuclear systems vary over a wide range. Studying density dependence of symmetry energy is thus a major topic of research in nuclear physics. Density dependence of symmetry energy is primarily characterized by three empirical quantities defined for infinite nuclear matter namely, symmetry energy coefficient J, slope parameter L and curvature parameter K_sym ; all of these quantities pertaining to saturation density \rho_0 of infinite nuclear matter. Since nuclear matter is not accessible in laboratories, one needs to find suitable experimental observables to constrain the values of J, L or K_sym. Though, J is quite precisely known from the experimental data on binding energies of nuclei, it is not quite the case for L or K_sym. This problem is addressed in this thesis using mean field models.