Toward a gravitational self-force-informed effective-one-body waveform model for nonprecessing, eccentric, large-mass-ratio inspirals
Alessandro Nagar, Simone Albanesi
Abstract
Building upon several recent advances in the developmentof effective-one-body (EOB) models for spin-aligned eccentric binaries with individual masses $({m}_{1},{m}_{2})$, we introduce a new EOB waveform model that aims at describing inspiraling binaries in the large mass-ratio regime, ${m}_{1}\ensuremath{\gg}{m}_{2}$. The model exploits the current state-of-the-art TEOBResumS-DALI model for eccentric binaries, but the standard EOB potentials $(A,\overline{D},Q)$, informed by numerical relativity (NR) simulations, are replaced with the corresponding functions that are linear in the symmetric mass ratio $\ensuremath{\nu}\ensuremath{\equiv}{m}_{1}{m}_{2}/({m}_{1}+{m}_{2}{)}^{2}$ taken at 8.5PN (Post-Newtonian) accuracy. To improve their strong-field behavior, these functions are (i) suitably factorized and resummed using Pad\'e approximants and (ii) additionally effectively informed to state-of-the-art numerical results obtained by gravitational self-force theory (GSF). For simplicity, the spin sector of the model is taken to be the one of TEOBResumS-DALI, though removing the NR-informed spin-orbit effective corrections. We propose the current GSF-informed EOB framework as a conceptually complete analytical tool to generate waveforms for eccentric extreme (and intermediate) mass ratio inspirals for future gravitational wave detectors.