Gravitational wave emission and spindown of young pulsars

TL;DR

This paper analyzes the gravitational wave emission and spin-down of young pulsars, showing that r-modes can explain observed pulsar frequencies and are promising sources for gravitational wave detection, with strain amplitude largely independent of microphysics.

Contribution

It provides a semi-analytic framework to assess r-mode effects on pulsar spin-down and gravitational waves, highlighting their viability as gravitational wave sources and the insensitivity of certain predictions to microphysics.

Findings

R-modes can explain pulsar spin-down within certain amplitudes.

Gravitational wave strain amplitude is independent of microphysics.

Advanced LIGO can detect several young neutron stars with r-mode emissions.

Abstract

The rotation frequencies of young pulsars are systematically below their theoretical Kepler limit. R-modes have been suggested as a possible explanation for this observation. With the help of semi-analytic expressions that make it possible to assess the uncertainties of the r-mode scenario due to the impact of uncertainties in underlying microphysics, we perform a quantitative analysis of the spin-down and the emitted gravitational waves of young pulsars. We find that the frequency to which r-modes spin down a young neutron star is surprisingly insensitive both to the microscopic details and the saturation amplitude. Comparing our result to astrophysical data, we show that for a range of sufficiently large saturation amplitudes r-modes provide a viable spindown scenario and that all observed young pulsars are very likely already outside the r-mode instability region. Therefore the most promising sources for gravitational wave detection are unobserved neutron stars associated with recent supernovae, and we find that advanced LIGO should be able to see several of them. We find the remarkable result that the gravitational wave strain amplitude is completely independent of both the r-mode saturation amplitude and the microphysics, and depends on the saturation mechanism only within some tens of per cent. However, the gravitational wave frequency depends on the amplitude and we provide the required expected timing parameter ranges to look for promising sources in future searches.