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Gravitational Radiation from Rapidly Rotating Nascent Neutron Stars

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arxiv astro-ph/9408053 v1 pith:WOC3CSL7 submitted 1994-08-17 astro-ph

Dong Lai , Stu Shapiro This is my paper · ORCID
classification astro-ph
keywords starwavegravitationalneutronincreasesrapidlyrotatingzero
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abstract

We study the secular evolution and gravitational wave signature of a newly-formed, rapidly rotating neutron star. The neutron star may arise from core collapse in a massive star or from the accretion-induced collapse of a white dwarf. After a brief dynamical phase, the nascent neutron star settles into an axisymmetric, secularly unstable equilibrium state. Gravitational radiation drives the star to a nonaxisymmetric, stationary equilibrium configuration via the bar-mode instability. The emitted quasi-periodic gravitational waves have a unique signature: the wave frequency sweeps downward from a few hundred Hertz to zero, while the wave amplitude increases from zero to a maximum and then decays back to zero. Such a wave signal could be detected by broad-band gravitational wave interferometers currently being constructed. We also characterize two other types of gravitational wave signals that could arise in principle from a rapidly rotating, secularly unstable neutron star: a high-frequency ($f\go 1000$ Hz) wave which increases the pattern-speed of the star, and a wave that actually increases the angular momentum of the star.

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Cited by 2 Pith papers

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  1. kiloHertz gravitational waves from binary neutron star remnants: time-domain model and constraints on extreme matter

    gr-qc 2019-08 conditional novelty 7.0 of 10

    A phase-coherent time-domain model for kilohertz postmerger gravitational waves from neutron star remnants is introduced, with injection studies indicating postmerger detection at SNR around 8.5 and radius constraints...

  2. All-sky search for long-duration gravitational-wave transients in the first part of the fourth LIGO-Virgo-KAGRA Observing run

    gr-qc 2025-07 accept novelty 6.0 of 10

    No long-duration gravitational-wave transients were found in O4a data; 50% efficiency amplitude limits improved by about 30% over O3, and eccentric CBC rate limits improved by factors of 2-7.

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