Gravitational waves from freely precessing neutron stars

TL;DR

This paper models gravitational wave emissions from freely precessing neutron stars, estimating their strength and assessing detectability, concluding that such signals are unlikely to be observed by current interferometers.

Contribution

It provides a detailed model of gravitational wave emission from precessing neutron stars considering internal dissipation and astrophysical mechanisms, evaluating their detectability.

Findings

Precession angles are rapidly damped in oblate stars due to internal dissipation.

Astrophysical mechanisms considered are too weak or infrequent for detection.

Free precession is unlikely to be detected by upcoming laser interferometers.

Abstract

In this paper we model the gravitational wave emission of a freely precessing neutron star. The aim is to estimate likely source strengths, as a guide for gravitational wave astronomers searching for such signals. We model the star as a partly elastic, partly fluid body with quadrupolar deformations of its moment of inertia tensor. The angular amplitude of the free precession is limited by the finite breaking strain of the star's crust. The effect of internal dissipation on the star is important, with the precession angle being rapidly damped in the case of a star with an oblate deformation. We then go on to study detailed scenarios where free precession is created and/or maintained by some astrophysical mechanism. We consider the effects of accretion torques, electromagnetic torques, glitches and stellar encounters. We find that the mechanisms considered are either too weak to lead to a signal detectable by an Advanced LIGO interferometer, or occur too infrequently to give a reasonable event rate. We therefore conclude that, using our stellar model at least, free precession is not a good candidate for detection by the forthcoming laser interferometers.