Could the stochastic gravitational wave background from newborn magnetars be detected by the advanced LIGO and Einstein Telescope?

TL;DR

This study evaluates the potential detectability of the stochastic gravitational wave background from newborn magnetars by advanced LIGO and Einstein Telescope, considering different formation mechanisms and their magnetic and spin properties.

Contribution

It introduces a comprehensive analysis of the SGWB from newborn magnetars across three formation scenarios, incorporating novel correlations and distributions of initial magnetic fields and spins.

Findings

SGWB from newborn magnetars is likely undetectable by aLIGO and ET.

Signal-to-noise ratios are below detection thresholds for all considered mechanisms.

Different formation scenarios significantly affect the predicted gravitational wave background.

Abstract

Newborn magnetars are important gravitational wave sources due to their ultra-strong magnetic fields and fast spins, and the entire population in the Universe may significantly contribute to the stochastic gravitational wave background (SGWB). In this work, we investigate the SGWB from newborn magnetars and assess its detectability by the advanced LIGO (aLIGO) and Einstein Telescope (ET) based on three typical formation mechanisms of magnetars, i.e., the $\alpha-\Omega$ dynamo, convective dynamo, and magnetic flux conservation. For the two dynamo scenarios, when calculating the SGWB, we creatively incorporate the anti-correlations between the magnetic fields and initial spin periods $P_{\rm i}$ with the initial dipole-field distribution of newborn magnetars. For the flux-conservation scenario, a bimodal lognormal form is adopted to describe the distribution of initial dipole fields, and all magnetars are assumed to have the same $P_{\rm i}$. Our results show that the SGWB from newborn magnetars may be undetectable by the aLIGO and ET if the magnetars are formed due to these mechanisms since the signal-to-noise ratio of the SGWB with respect to the ET for an observation time of one year is only 0.37 for the $\alpha-\Omega$ dynamo, $3\times10^{-4}$ for the convective dynamo, and at most 0.21 for the flux conservation.