Abstract
In one of our previous articles we have considered the role of a time dependent magnetic ellipticity on the pulsars’ braking indices and on the putative gravitational waves these objects can emit. Since only nine of more than 2000 known pulsars have accurately measured braking indices, it is of interest to extend this study to all known pulsars, in particular as regards gravitational wave generation. To do so, as shown in our previous article, we need to know some pulsars’ observable quantities such as: periods and their time derivatives, and estimated distances to the Earth. Moreover, we also need to know the pulsars’ masses and radii, for which we are adopting current fiducial values. Our results show that the gravitational wave amplitude is at best h sim 10^{-28}. This leads to a pessimistic prospect for the detection of gravitational waves generated by these pulsars, even for Advanced LIGO and Advanced Virgo, and the planned Einstein Telescope, if the ellipticity has a magnetic origin.
Highlights
It is well known that, besides compact binaries, rapidly rotating neutron stars are promising sources of gravitational waves (GWs) which could be detected in a near future by advanced LIGO and advanced VIRGO (AdV), and by the planned Einstein Telescope (ET)
We extend our previous studies [6] in which we considered the role of magnetic ellipticity on the braking index and on the pulsar distortion
It is well known that, for strong magnetic fields (∼1012 to 1015 G), the equilibrium configuration of a neutron star can be distorted by magnetic tension
Summary
It is well known that, besides compact binaries, rapidly rotating neutron stars are promising sources of gravitational waves (GWs) which could be detected in a near future by advanced LIGO (aLIGO) and advanced VIRGO (AdV), and by the planned Einstein Telescope (ET). With εB in hands, we can calculate the GW amplitudes for all pulsars with known P, P , and their distances to the Earth. In this regard it is worth mentioning that the distance to these sources has been established, there are observational uncertainties in its determination, which are not taken into account in the present paper.
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