  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).
