Tail-induced spin-orbit effect in the gravitational radiation of compact binaries

TL;DR

This paper enhances the understanding of spin-orbit tail effects in gravitational waves from compact binaries by computing higher-order post-Newtonian terms, improving waveform models for better detection and analysis.

Contribution

It derives spin-orbit tail effects at 3PN order in energy flux and 2.5PN and 3PN orders in wave polarizations, advancing analytical gravitational wave modeling.

Findings

Derived spin-orbit tail effects at 3PN order in energy flux.

Computed spin-orbit tail effects at 2.5PN and 3PN orders in wave polarizations.

Improved accuracy of gravitational waveform phasing for binary inspirals.

Abstract

Gravitational waves contain tail effects which are due to the back-scattering of linear waves in the curved space-time geometry around the source. In this paper we improve the knowledge and accuracy of the two-body inspiraling post-Newtonian (PN) dynamics and gravitational-wave signal by computing the spin-orbit terms induced by tail effects. Notably, we derive those terms at 3PN order in the gravitational-wave energy flux, and 2.5PN and 3PN orders in the wave polarizations. This is then used to derive the spin-orbit tail effects in the phasing through 3PN order. Our results can be employed to carry out more accurate comparisons with numerical-relativity simulations and to improve the accuracy of analytical templates aimed at describing the whole process of inspiral, merger and ringdown.