A Theoretical Study of the Equation of States for Crustal Matter of Strongly Magnetized Neutron Stars

TL;DR

This paper explores the properties and equations of state of dense crustal matter in strongly magnetized neutron stars using relativistic models and compares different nuclear mass formulas, revealing significant changes in crustal properties.

Contribution

It provides a theoretical analysis of crustal matter in magnetars using relativistic Thomas-Fermi models and compares various nuclear equations of state.

Findings

Significant changes in crustal matter properties under strong magnetic fields.

Differences observed between outer and inner crust properties.

Impact of nuclear mass formulas on crustal matter characteristics.

Abstract

We have investigated some of the properties of dense sub-nuclear matter at the crustal region (both the outer crust and the inner crust region) of a magnetar. The relativistic version of Thomas-Fermi (TF) model is used in presence of strong quantizing magnetic field for the outer crust matter. The compressed matter in the outer crust, which is a crystal of metallic iron, is replaced by a regular array of spherically symmetric Wigner-Seitz (WS) cells. In the inner crust region, a mixture of iron and heavier neutron rich nuclei along with electrons and free neutrons has been considered. Conventional Harrison-Wheeler (HW) and Bethe-Baym-Pethick (BBP) equation of states are used for the nuclear mass formula. A lot of significant changes in the characteristic properties of dense crustal matter, both at the outer crust and the inner crust, have been observed.