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

TL;DR

This paper details the inclusion of adiabatic tidal effects into gravitational waveforms for non-spinning compact binaries up to 2.5 post-Newtonian order, enhancing waveform modeling accuracy.

Contribution

It introduces a method to incorporate tidal effects into gravitational wave amplitude and phase models up to 2.5PN order, suitable for effective-one-body frameworks.

Findings

Derived tidal contributions to waveform amplitude and phase.

Provided explicit formulas for waveform modes and energy flux.

Enhanced accuracy of gravitational waveform models for binary neutron stars.

Abstract

This paper describes the different steps to include the adiabatic tidal effects to the gravitational waveform amplitude for quasi-circular non-spinning 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 -2, parametrized by the two numbers $(\ell,m)$, 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. The results presented in this article are collected in an ancillary file.