Stochastic background of gravitational waves generated by a cosmological population of young, rapidly rotating neutron stars

Details Stochastic background of gravitational waves generated by a cosmological population of young, rapidly rotating neutron stars Stochastic background of gravitational waves generated by a cosmological population of young, rapidly rotating neutron stars

1998-06-26

arxiv.org/abs/astro-ph/9806357v2

Mon.Not.Roy.Astron.Soc. 303 (1999) 258

Astronomy and Astrophysics

Astrophysics

8 pages, 9 figures, accepted for publication in MNRAS

Scientific paper

10.1046/j.1365-8711.1999.02207.x

We estimate the spectral properties of the stochastic background of gravitational radiation emitted by a cosmological population of hot, young, rapidly rotating neutron stars. Their formation rate as a function of redshift is deduced from an observation-based determination of the star formation history in the Universe, and the gravitational energy is assumed to be radiated during the spin-down phase associated to the newly discovered r-mode instability. We calculate the overall signal produced by the ensemble of such neutron stars, assuming various cosmological backgrounds. We find that the spectral strain amplitude has a maximum $\approx (2-4)\times 10^{-26} {Hz}^{-1/2}$, at frequencies $\approx (30-60)$ Hz, while the corresponding closure density, $h^2 \Omega_{GW}$, has a maximum amplitude plateau of $\approx (2.2-3.3) \times 10^{-8}$ in the frequency range $(500-1700)$ Hz. We compare our results with a preliminary analysis done by Owen et al. (1998), and discuss the detectability of this background.

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