We carry out the study of finite nuclei, infinite nuclear matter, and neutron star properties with
the newly developed relativistic force, the Institute of Physics Bhubaneswar-I (IOPB-I). Using …

The impact of anisotropic pressure models in neutron stars (NSs) is increasing their
compactness. Therefore, for the relatively soft NS equation of state (EOS), we can still obtain …

We systematically study the tidal deformability for neutron and hyperon stars using
relativistic mean field equations of state (EOSs). The tidal effect plays an important role …

A new parameter set is generated for finite and infinite nuclear system within the effective
field theory motivated relativistic mean field (ERMF) formalism. The isovector part of the …

Even though the crystallized nature of the neutron star crust plays a pivotal role in describing
various fascinating astrophysical observations, its microscopic structure is not fully …

The rotating neutron-star properties are studied to investigate a phase transition to quark
matter. The density-dependent relativistic mean-field model (DD-RMF) is employed to study …

We use the effective relativistic mean-field (E-RMF) model to study the crustal properties of
the neutron star. The unified equations of state (EoS) are constructed using recently …

The recently published CREX results suggest a rather peculiar picture for the density
dependence of the symmetry energy. Whereas PREX favors a large neutron skin thickness …

An isovector–scalar meson is incorporated self-consistently into the quark–meson coupling
description of nuclear matter, and its most prominent effects on the structure of neutron stars …

The structural and decay properties of the ground state of recently discovered neutron-
deficient 207 Th and remeasured 208 Th isotopes Yang et al.(2022)[26] is examined using …