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We develop the foundations of an effective-one-body (EOB) model for eccentricbinary coalescences that includes the conservative dynamics, radiationreaction, and gravitational waveform modes from the inspiral and themerger-ringdown signals. We use the same approach as is commonly employed inblack-hole perturbation theory by introducing a relativistic parameterizationof the dynamics that is defined by the orbital geometry and consists of a setof phase variables and quantities that evolve only due to gravitationalradiation reaction. Specializing to nonspinning binaries, we derive the EOBevolution equations and compute the binary's radiative multipole moments thatdetermine the gravitational waves through a decomposition into the fundamentalfrequencies of the motion. The major differences between our treatment and thequasi-Keplerian approach often used in post-Newtonian (PN) calculations arethat the orbital parameters describe strong-field dynamics, and that expressingthe multipole moments in terms of the frequencies simplifies the calculationsand also results in an unambiguous orbit-averaging operation. While ourdescription of the conservative dynamics is fully relativistic, we limitexplicit derivations in the radiative sector to 1.5PN order for simplicity.This already enables us to establish methods for computing both instantaneousand hereditary contributions to the gravitational radiation in EOB coordinatesthat have straightforward extensions to higher PN order. The weak-field, smalleccentricity limit of our results for the orbit-averaged fluxes of energy andangular momentum agrees with known PN results when expressed in terms ofgauge-invariant quantities. We further address considerations for the numericalimplementation of the model and the completion of the waveforms to include themerger and ringdown signals, and provide illustrative results.

Foundations of an effective-one-body model for coalescing binaries on eccentric orbits