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arXiv · gr-qc/9804044

Gravitational waves from hot young rapidly rotating neutron stars

Benjamin J. Owen·Lee Lindblom·Curt Cutler·Bernard F. Schutz·Alberto Vecchio·Nils Andersson
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Abstract

Gravitational radiation drives an instability in the r-modes of young rapidly rotating neutron stars. This instability is expected to carry away most of the angular momentum of the star by gravitational radiation emission, leaving a star rotating at about 100 Hz. In this paper we model in a simple way the development of the instability and evolution of the neutron star during the year-long spindown phase. This allows us to predict the general features of the resulting gravitational waveform. We show that a neutron star formed in the Virgo cluster could be detected by the LIGO and VIRGO gravitational wave detectors when they reach their ``enhanced'' level of sensitivity, with an amplitude signal-to-noise ratio that could be as large as about 8 if near-optimal data analysis techniques are developed. We also analyze the stochastic background of gravitational waves produced by the r-mode radiation from neutron-star formation throughout the universe. Assuming a substantial fraction of neutron stars are born with spin frequencies near their maximum values, this stochastic background is shown to have an energy density of about 10^-9 of the cosmological closure density, in the range 20 Hz to 1 kHz. This radiation should be detectable by ``advanced'' LIGO as well.

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Benjamin J. Owen, Lee Lindblom, Curt Cutler, Bernard F. Schutz, Alberto Vecchio, Nils Andersson. 1998-05-04. Gravitational waves from hot young rapidly rotating neutron stars. https://doi.org/10.1103/physrevd.58.084020

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