Description
Abstract: Within the effective-one-body (EOB) formalism, the losses of energy and angular
momentum of a binary due to the emission of gravitational waves (GWs) are
modeled through a radiation-reaction (RR) force entering the
EOB equations of motion.
An accurate prescription for the EOB RR force is crucial, as it directly
determines the phase evolution of the binary, to which GW detectors are
particularly sensitive.
Inaccuracies in the RR force can therefore lead to systematic biases in the
estimation of the source parameters.
In this talk, I will describe how post-Newtonian results for the energy and
angular momentum fluxes are used, via flux-balance laws, to construct an
EOB radiation-reaction force, and I will discuss the additional difficulties that
arise when considering binaries on generic (non-circular) orbits.
I will then explain how these results are resummed and incorporated into
state-of-the-art EOB waveform models for eccentric binaries.
Finally, I will comment on the challenges involved in comparing different
eccentric waveform models, particularly in relation to eccentric numericalrelativity
simulations.
