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

This paper describes the different steps to include the adiabatic tidal effects to the gravitational waveform amplitude for quasicircular nonspinning compact binaries up to the second-and-a-half post-Newtonian (PN) order. The amplitude, that relates the two gravitational wave polarizations, is decomposed onto the basis of spin-weighted spherical harmonics of spin $\ensuremath{-}2$, parametrized by the two numbers $(\ensuremath{\ell},m)$, where the modes of the waveform correspond to the coefficients of the decomposition. These modes are readily computed from the radiative multipole moments. They can be expressed in a PN-expanded form as well as in a factorized form, suitable to be directly included in effective-one-body models to describe more accurately the waveform of binary neutron stars. We also provide the energy flux and phasing evolution in time and frequency domain.

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Publication Details

Journal
Physical review. D/Physical review. D.
Published
2025-04-16
DOI
https://doi.org/10.1103/physrevd.111.084043
Citations
4
Primary Topic
Pulsars and Gravitational Waves Research
Type
article
Field-Weighted Citation Impact
4.62

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article

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

Quentin Henry, Laura Bernard, Eve Dones
4 citations
Physical review. D/Physical review. D.
Pulsars and Gravitational Waves Research
4.62
article

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

Quentin Henry, Laura Bernard, Eve Dones
article en
4 citations

Abstract

This paper describes the different steps to include the adiabatic tidal effects to the gravitational waveform amplitude for quasicircular nonspinning compact binaries up to the second-and-a-half post-Newtonian (PN) order. The amplitude, that relates the two gravitational wave polarizations, is decomposed onto the basis of spin-weighted spherical harmonics of spin $\ensuremath{-}2$, parametrized by the two numbers $(\ensuremath{\ell},m)$, where the modes of the waveform correspond to the coefficients of the decomposition. These modes are readily computed from the radiative multipole moments. They can be expressed in a PN-expanded form as well as in a factorized form, suitable to be directly included in effective-one-body models to describe more accurately the waveform of binary neutron stars. We also provide the energy flux and phasing evolution in time and frequency domain.

Physical review. D/Physical review. D.Vol. 111(8)
Université Paris Cité (FR), Université Paris Sciences et Lettres (FR), Observatoire de Paris (FR), Laboratoire Univers et Théories (FR), Max Planck Institute for Gravitational Physics (DE), Fundació Universitat-Empresa de les Illes Balears (ES), Universitat de les Illes Balears (ES)
Innovation, Science and Economic Development Canada, European Commission, Agence Nationale de la Recherche, Max-Planck-Gesellschaft, Centre National de la Recherche Scientifique, Ministerio de Ciencia e Innovación, Universitat de les Illes Balears, Institut Périmètre de physique théorique, Ministry of Colleges and Universities, Horizon 2020 Framework Programme, European Regional Development Fund, Agencia Estatal de Investigación, HORIZON EUROPE Marie Sklodowska-Curie Actions
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Openalex Percentile: Top 6%
Pulsars and Gravitational Waves Research
4.62
DOISourceOpenAlex
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