Gravitational waves from hot young rapidly rotating neutron stars
Apr, 1998
15 pages
Published in:
- Phys.Rev.D 58 (1998) 084020
e-Print:
- gr-qc/9804044 [gr-qc]
Report number:
- GRP-496
View in:
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Abstract: (arXiv)
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.- n: matter
- gravitational radiation: stability
- background: stochastic
- velocity
- temperature dependence
- gravitational radiation: measurement
- counters and detectors
- interference: laser
- numerical calculations
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