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TIDAL AND TIDAL-RESONANT EFFECTS IN COALESCING BINARIES

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arxiv gr-qc/9502034 v1 pith:ROF5SS2M submitted 1995-02-17 gr-qc

Kostas D. Kokkotas , Gerhard Schaefer This is my paper · ORCID
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abstract

Tidal and tidal-resonant effects in coalescing compact binary systems are investigated by direct numerical integration of the equations of motion. For the stars polytropic models are used. The tidal effects are found to be dominated by the (non-resonant) $f$-modes. The effect of the $g$-mode-tidal resonances is obtained. The tidal interaction is shown to be of interest especially for low-mass binaries. There exists a characteristic final plunge orbit beyond which the system cannot remain stable even if radiation reaction is not taken into account; in agreement with results obtained by Lai et al. \shortcite{Lai93}. The importance of the investigated effects for the observation of gravitational waves on Earth is discussed.

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Cited by 4 Pith papers

Reviewed papers in the Pith corpus that reference this work. Sorted by Pith novelty score. Full citation record

  1. A Bound on the Dynamical Love Number

    gr-qc 2026-07 conditional novelty 7.0 of 10

    Schwarz–Pick applied to the rescaled retarded tidal response bounds dynamical Love numbers for neutron stars by the static Love number and spectral gap, and constrains black-hole tidal heating.

  2. Universal Relations with Dynamical Tides

    gr-qc 2025-11 unverdicted novelty 6.0 of 10

    New quasi-universal relations connect static tidal deformability Λ⁰ to its dynamical correction Λ² and to Mω* with equation-of-state scatter below 5% and 2.8% respectively across 59 models.

  3. The error budget of binary neutron star merger simulations for configurations with high spin

    gr-qc 2025-06 accept novelty 6.0 of 10

    For highly spinning (chi=0.5) binary neutron stars, evolution code choice is the largest numerical waveform error, and current analytical models disagree with numerical relativity beyond that error after the stars touch.

  4. Resonances of compressible stars in precessing orbits around a spinning black hole

    astro-ph.HE 2025-02 conditional novelty 4.0 of 10

    The resonance found for incompressible stars persists for compressible polytropic stars with stiff equations of state, but its radius shrinks as the polytropic index grows, and the second-order resonance disappears for n=2.

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