Modelling magnetically deformed neutron stars

TL;DR

This paper develops a formalism to model magnetically deformed neutron stars with realistic equations of state, focusing on dipolar magnetic fields and their gravitational wave emission implications for detectors like LIGO and VIRGO.

Contribution

It introduces a new formalism for modeling magnetic deformations in neutron stars using realistic equations of state and dipolar magnetic fields.

Findings

Calculated internal magnetic fields consistent with neutron star models.

Determined star deformations due to magnetic fields.

Discussed implications for gravitational wave detection.

Abstract

Rotating deformed neutron stars are important potential sources for groundbased gravitational-wave interferometers such as LIGO, GE0600 and VIRGO. One mechanism that may lead to significant non-asymmetries is the internal magnetic field. It is well known that a magnetic star will not be spherical and, if the magnetic axis is not aligned with the spin axis, the deformation will lead to the emission of gravitational waves. The aim of this paper is to develop a formalism that would allow us to model magnetically deformed stars, using both realistic equations of state and field configurations. As a first step, we consider a set of simplified model problems. Focusing on dipolar fields, we determine the internal magnetic field which is consistent with a given neutron star model. We then calculate the associated deformation. We conclude by discussing the relevance of our results for current gravitational-wave detectors and future prospects.