Third post-Newtonian spin-orbit effect in the gravitational radiation flux of compact binaries

TL;DR

This paper derives the third post-Newtonian order spin-orbit tail effects in gravitational wave fluxes from compact binaries, enhancing the precision of waveform models for gravitational wave detection.

Contribution

It provides the first derivation of spin-orbit tail effects at 3PN order, improving analytical gravitational wave templates for inspiraling compact binaries.

Findings

Derived the 3PN spin-orbit tail effects in gravitational-wave flux.

Updated the phasing formula to include these effects.

Facilitates more accurate gravitational wave data analysis.

Abstract

Gravitational waves contain tail effects that are due to the backscattering of linear waves in the curved space-time geometry around the source. The knowledge as well as the accuracy of the two-body inspiraling post-Newtonian (PN) dynamics and of the gravitational-wave signal has been recently improved, notably by computing the spin-orbit (SO) terms induced by tail effects in the gravitational-wave energy flux at the 3PN order. Here we sketch this derivation, which yields the phasing formula including SO tail effects through the same 3PN order. Those results can be employed to improve the accuracy of analytical templates aimed at describing the whole process of inspiral, merger, and ringdown.