The gravitational wave signal from isolated objects

TL;DR

This paper explores gravitational wave emissions from isolated neutron stars with deformations, using observational data and population synthesis to estimate GW luminosity ranges, aiding future detections by LIGO.

Contribution

It introduces a method combining observational data and binary population synthesis to estimate gravitational wave emissions from deformed isolated neutron stars.

Findings

GW luminosity ranges from 10^{40} to 10^{55} erg/s

Deformed neutron stars can be significant GW sources

Method can be confirmed by future LIGO observations

Abstract

According to the theoretical study, a deformation object (e.g., a spinning non-axisymmetric pulsar star) will radiate a gravitational wave (GW) signal during an accelaration motion process by LIGO science project. These types of disturbance sources with a large bump or dimple on the equator would survive and be identifiable as GW sources. In this work, we aim to provide a method for exploring GW radiation from isolated neutron stars (NSs) with deformation state using some observational results, which can be confirmed by the next LIGO project. Combination with the properties in observation results (e.g., PSR J1748-2446, PSR 1828-11 and Cygnus X-1), based on a binary population synthesis (BPS) approach we give a numerical GW radiation under the assumption that NS should have non-axisymmetric and give the results of energy spectrum. We find that the GW luminosity of $L_{GW}$ can be changed from about $10^{40}\rm erg/s$-- $10^{55}\rm erg/s$.