Exploration of Nuclear Matter Properties and Related Thermodynamical Aspects

TL;DR

This paper investigates how nuclear matter properties vary under different conditions like temperature, density, and magnetic fields, using the effective relativistic mean field model to understand phenomena in neutron stars and heavy-ion collisions.

Contribution

It provides a comprehensive analysis of nuclear matter properties across various conditions using the E-RMF model, highlighting model dependencies and phase diagram features.

Findings

Nuclear matter properties are highly sensitive to EoS parameters.

Phase diagram features depend on temperature, density, and magnetic field.

Model predictions inform understanding of neutron star characteristics.

Abstract

In this study, my main goal is to examine the nuclear matter properties across a wide range of conditions, such as temperature, density, asymmetry, pressure, and magnetic field. Understanding the effect of these factors on nuclear matter is essential, given their relevance in various phenomena such as heavy-ion collisions, neutron stars, and supernovae. However, due to the absence of a fundamental nuclear theory, we must rely on models to describe the nuclear matter. Predicted properties like neutron star mass-radius relationships, tidal deformability, structure, critical points in the nuclear matter phase diagram etc. depend on the chosen model. This dependence arises because key parameters characterizing any nuclear model or equation of state (EoS) are not precisely known. Therefore, it is crucial to investigate how nuclear matter properties behave under various conditions and in relation to different EoS parameters. To accomplish this, I have examined three distinct forms of nuclear matter: infinite nuclear matter, finite nuclei, and neutron stars, using the effective relativistic mean field model (E-RMF).