Description
Abstract: Next-generation gravitational wave detectors, such as LISA, the Einstein
Telescope, and Cosmic Explorer, will require accurate modelling of long-lived black
hole binary signals, including those with orbital eccentricity. A major challenge in
using eccentric effective-one-body (EOB) models for parameter estimation is the
high computational cost of evolving long-lived eccentric dynamics. We address this
by first recasting the EOB equations of motion using the method of osculating
orbital elements and then applying near-identity averaging transformations during
the inspiral phase.
By implementing these transformations up to second post-adiabatic order, we obtain
averaged equations of motion that faithfully capture the long-term dynamics of
comparable-mass systems. This approach eliminates the need to resolve rapidly
oscillating orbital dynamics, reducing the cost of the dynamics by a factor of the
mass ratio and reducing the overall cost of waveform generation even for
comparable mass systems.
