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We compute the next-to-next-to-leading order spin-orbit contributions in thetotal energy flux emitted in gravitational waves by compact binary systems.Such contributions correspond to the post-Newtonian order 3.5PN for maximallyspinning compact objects. Continuing our recent work on thenext-to-next-to-leading spin-orbit terms at 3.5PN order in the equations ofmotion, we obtain the spin-orbit terms in the multipole moments of the compactbinary system up to the same order within the multipolar post-Newtonian wavegeneration formalism. Our calculation of the multipole moments is valid forgeneral orbits and in an arbitrary frame; the moments are then reduced to thecenter-of-mass frame and the resulting energy flux is specialized toquasi-circular orbits. The test-mass limit of our final result for the fluxagrees with the already known Kerr black hole perturbation limit. Furthermorethe various multipole moments of the compact binary reduce in the one-body caseto those of a single boosted Kerr black hole. We briefly discuss theimplications of our result for the gravitational-wave flux in terms of thebinary's phase evolution, and address its importance for the future detectionand parameter estimation of signals in gravitational wave detectors.

Next-to-next-to-leading order spin-orbit effects in the gravitational wave flux and orbital phasing of compact binaries