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Tidal effects in the gravitational-wave phase evolution of compact binary systems to next-to-next-to-leading post-Newtonian order

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arxiv 2005.13367 v4 pith:6IYL64OR submitted 2020-05-27 gr-qc

Quentin Henry , Guillaume Faye , Luc Blanchet This is my paper · ORCID
classification gr-qc
keywords ordertidalenergysystembinarycompactcontributionseffects
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We compute the gravitational-wave (GW) energy flux up to the next-to-next-to-leading (NNL) order of tidal effects in a spinless compact binary system on quasi-circular orbits. Starting from an effective matter action, we obtain the stress-energy tensor of the system, which we use in a GW generation formalism based on multipolar-post-Minkowskian (MPM) and post-Newtonian (PN) approximations. The tidal contributions to the multipole moments of the system are first obtained, from which we deduce the instantaneous GW energy flux to NNL order (formally 7PN order). We also include the remaining tidal contributions of GW tails to the leading (formally 6.5PN) and NL (7.5PN) orders. Combining it with our previous work on the conservative equations of motion (EoM) and associated energy, we get the GW phase and frequency evolution through the flux-balance equation to the same NNL order. These results extend and complete several preceding results in the literature.

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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. Quadrupolar tidal effects destroy the integrability of black hole geodesics: analytic proof and numerical evidence of chaos

    gr-qc 2026-07 accept novelty 7.0 of 10

    Leading-order tidally induced quadrupoles destroy Kerr geodesic integrability: no polynomial deformation of the Carter constant is conserved for generic Love couplings and Kerr spin.

  2. Tidal contributions to the full gravitational waveform to the second-and-a-half post-Newtonian order

    gr-qc 2024-12 conditional novelty 7.0 of 10

    Tidal contributions to all gravitational waveform amplitude modes up to l=7 are derived to 2.5PN for quasi-circular non-spinning compact binaries, with flux and phasing provided at the same order.

  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. Data-driven approach for extracting tidal information from neutron star binary mergers observed with the Einstein Telescope

    gr-qc 2025-01 conditional novelty 6.0 of 10

    A simulation study showing that the tidal phase of neutron-star mergers can be inferred directly from Einstein Telescope data by fitting six free polynomial coefficients and combining posteriors across events.

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