Structure of ultra-magnetised neutron stars

TL;DR

This paper reviews methods for modeling strongly magnetized neutron stars within general relativity, emphasizing the importance of non-spherical solutions and presenting a universal magnetic field profile applicable to astrophysical observations.

Contribution

It introduces a self-consistent formalism for rotating, magnetized neutron star models beyond spherical symmetry, including a universal magnetic field profile for nuclear physics applications.

Findings

Full numerical solutions reveal magnetic field effects on star radius and crust thickness.

A universal magnetic field profile is proposed for neutron star studies.

The methodology aids in interpreting multi-messenger astrophysical data.

Abstract

In this review we discuss self-consistent methods to calculate the global structure of strongly magnetised neutron stars within the general-relativistic framework. We outline why solutions in spherical symmetry cannot be applied to strongly magnetised compact stars, and elaborate on a consistent formalism to compute rotating magnetised neutron star models. We also discuss an application of the above full numerical solution for studying the influence of strong magnetic fields on the radius and crust thickness of magnetars. The above technique is also applied to construct a "universal" magnetic field profile inside the neutron star, that may be useful for studies in nuclear physics. The methodology developed here is particularly useful to interpret multi-messenger astrophysical data of strongly magnetised neutron stars.