Constraining the ellipticity of millisecond pulsars with observed spin-down rates

TL;DR

This paper constrains the ellipticity of millisecond pulsars using observed spin-down rates, estimating their gravitational wave emission potential and electrical resistivities, and discusses detectability with future GW detectors.

Contribution

It introduces a method to estimate MSP ellipticities and resistivities based on spin-down rates, linking GW emission to accretion processes and magnetic field configurations.

Findings

Ellipticities of MSPs are estimated to be between 0.9 and 23.4 times 10^{-9}.

Electrical resistivities are in the range 1.2 to 15.3 times 10^{-31} seconds.

Characteristic GW strains are beyond current detector sensitivity but may be detectable with future observatories.

Abstract

A spinning neutron star (NS) that is asymmetric with respect to its spin axis can emit continuous gravitational wave (GW) signals. The spin frequencies and their distribution of radio millisecond pulsars (MSPs) and accreting MSPs provide some evidences of GW radiation, and MSPs are ideal probes detecting high frequency GW signals. It is generally thought that MSPs originate from the recycled process, in which the NS accretes the material and angular momentum from the donor star. The accreted matter would be confined at the polar cap zone by an equatorial belt of compressed magnetic field fixed in the deep crust of the NS, and yields "magnetic mountain". Based on an assumption that the spin-down rates of three transitional MSPs including PSR J1023+0038 are the combinational contribution of the accretion torque, the propeller torque, and the GW radiation torque, in this work we attempt to constrain the ellipticities of MSPs with observed spin-down rates. Assuming some canonical parameters of NSs, the ellipticities of three transitional MSPs and ten redbacks are estimated to be $\epsilon=(0.9-23.4)\times 10^{-9}$. The electrical resistivities of three transitional MSPs are also derived to be in the range $\eta=(1.2-15.3)\times 10^{-31}~\rm s$, which display an ideal power law relation with the accretion rate. The characteristic strains ($h_{\rm c}=(0.6-2.5)\times10^{-27}$) of GW signals emitting by these sources are obviously beyond the sensitivity scope of the aLIGO. We expect that the third-generation GW detectors like the Einstein Telescope can seize the GW signals from these sources in the future.