Volume 586, February 2016
|Number of page(s)||8|
|Published online||28 January 2016|
The stochastic background of gravitational waves due to the f-mode instability in neutron stars
1 Theoretical Astrophysics, IAAT, Eberhard-Karls University of Tübingen, 72076 Tübingen, Germany
2 Institute of Cosmology and Gravitation, University of Portsmouth, Burnaby Rd, Portsmouth, PO1 3FX, UK
Received: 14 August 2015
Accepted: 3 December 2015
This paper presents an estimate for the spectral properties of the stochastic background of gravitational waves emitted by a population of hot, young, rapidly rotating neutron stars throughout the Universe undergoing f-mode instabilities, formed through either core-collapse supernova explosions or the merger of binary neutron star systems. Their formation rate, from which the gravitational wave event rate is obtained, is deduced from observation-based determinations of the cosmic star formation rate. The gravitational wave emission occurs during the spin-down phase of the f-mode instability. For low magnetized neutron stars and assuming 10% of supernova events lead to f-mode unstable neutron stars, the background from supernova-derived neutron stars peaks at Ωgw ~ 10-9 for the l = m = 2f-mode, which should be detectable by cross-correlating a pair of second generation interferometers (e.g. Advanced LIGO/Virgo) with an upper estimate for the signal-to-noise ratio of ≈9.8. The background from supramassive neutron stars formed from binary mergers peaks at Ωgw ~ 10-10 and should not be detectable, even with third generation interferometers (e.g. Einstein Telescope).
Key words: cosmology: miscellaneous / gravitational waves / stars: neutron / stars: oscillations
© ESO, 2016
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