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

1998/06/30 by Valeria Ferrari, S. Matarrese, Sabino Matarrese +1 · 14 citations
Earth and Planetary Sciences · Physics and Astronomy · #Gamma-ray bursts and supernovae #Geophysics and Gravity Measurements #Pulsars and Gravitational Waves Research #astro-ph #gr-qc

paper · pdf · doi:10.1046/j.1365-8711.1999.02207.x

published as Mon.Not.Roy.Astron.Soc. 303 (1999) 258 · 8 pages, 9 figures, accepted for publication in MNRAS

arxiv created 1998/10/15 · arxiv updated 2009/11/30

Abstract

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 ≈ (2-4)× 10^-26 Hz^-1/2, at frequencies ≈ (30-60) Hz, while the corresponding closure density, h² Ω_GW, has a maximum amplitude plateau of ≈ (2.2-3.3) × 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.

Citations

• Gravitational Wave Background from a Cosmological Population of Core-Collapse Supernovae

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