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Gravitational waves from hot young rapidly rotating neutron stars

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arxiv gr-qc/9804044 v2 pith:MIOW5HQJ submitted 1998-04-20 gr-qc

Benjamin J. Owen , Lee Lindblom , Curt Cutler , Bernard F. Schutz , Alberto Vecchio , Nils Andersson This is my paper
classification gr-qc
keywords gravitationalneutronradiationstarinstabilityrotatingstarsbackground
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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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Cited by 4 Pith papers

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    gr-qc 2025-06 conditional novelty 7.0 of 10

    Using causal BDNK hydrodynamics, the authors derive coupled gravitational-wave and viscous-mode equations for slowly rotating stars and find superradiant amplification at low frequencies.

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    astro-ph.HE 2026-08 conditional novelty 6.0 of 10

    Using 3D supernova simulations, the authors predict that neutrino memory creates a gravitational wave background with Omega_GW around 1e-16 at 0.1 Hz, within reach of future space-based detectors.

  3. Search for continuous gravitational waves from the pulsar J0435+3233

    gr-qc 2026-07 accept novelty 6.0 of 10

    A LIGO O4a search for continuous gravitational waves from millisecond pulsar J0435+3233 finds no signal, setting h0<5.8×10^-27 at 95% confidence and an ellipticity limit of 1.6×10^-8.

  4. Inferring neutron star properties through gravitational waves from r-modes and their relativistic counterparts

    astro-ph.HE 2024-06 unverdicted novelty 4.0 of 10

    Two inference frameworks are developed for neutron star properties from r-mode gravitational waves, one assuming electromagnetic distance and the other estimating distance via universal relations plus an assumed equat...

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