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We leverage recent breakthrough calculations using second-order gravitationalself-force (2GSF) theory to improve both the gravitational-mode amplitudes andradiation-reaction force in effective-one-body~(EOB) waveform models. Weachieve this by introducing new calibration parameters in the SEOBNRv5HM modeamplitudes, and matching them to the newly available 2GSF energy-fluxmultipolar data for quasicircular nonspinning binary black holes. We find thatthis significantly improves the SEOBNRv5HM energy flux, when compared tonumerical-relativity (NR) simulations of binary black holes with mass ratiosbetween 1:1 and 1:20. Moreover, we find that, once the conservative part of theSEOBNRv5 dynamics is calibrated, the SEOBNRv5HM waveform model with 2GSFinformation reproduces the binding energy of NR simulations more accurately,providing a powerful check of the consistency and naturalness of the EOBapproach. While we only include nonspinning 2GSF information, the more accuratebinding energy and energy flux carry over to the SEOBNRv5 waveform models forspinning binary black holes. Thus, our results improve the latest generation ofSEOBNR waveform models (i.e., SEOBNRv5), which has been recently completed foruse in the upcoming fourth observing (O4) run of the LIGO-Virgo-KAGRACollaboration.

Enhancing the SEOBNRv5 effective-one-body waveform model with second-order gravitational self-force fluxes