Towards efficient Effective One Body models for generic, non-planar orbits

TL;DR

This paper introduces an efficient method to model the evolution of spins and orbital angular momentum in eccentric, precessing binary black hole systems, enhancing the Effective-One-Body framework for gravitational wave predictions.

Contribution

It presents a novel prescription for evolving spin vectors and orbital angular momentum in non-circular orbits, integrated into an EOB model for eccentric, precessing BBHs.

Findings

Negligible impact of non-circular spin evolution terms.

Validation against numerical relativity simulations shows high accuracy.

Model performs well in quasi-spherical limit with low mismatches.

Abstract

Complete waveform models able to account for arbitrary non-planar orbits represent a holy grail in current gravitational-wave astronomy. Here, we take a step towards this direction and present a simple yet efficient prescription to obtain the evolution of the spin vectors and of the orbital angular momentum along non-circularized orbits, that can be applied to any eccentric aligned-spins waveform model. The scheme employed is motivated by insights gained from the post-Newtonian (PN) regime. We investigate the phenomenology of the Euler angles characterizing the time-dependent rotation that connects the co-precessing frame to the inertial one, gauging the importance of non-circular terms in the evolution of the spins of a precessing binary. We demonstrate that such terms are largely negligible, irrespectively of the details of the orbit. Such insights are confirmed by studying the radiation-frame of a few eccentric, precessing numerical relativity (NR) simulations. Our investigations confirm that the usual "twisting" technique employed for quasi-spherical systems can be safely applied to non-circularized binaries. By then augmenting a state-of-the-art Effective-One-Body (EOB) model for non-circular planar orbits with the prescription discussed, we obtain an inspiral-merger-ringdown (IMR) model for eccentric, precessing binary black holes (BBHs). We validate the model in the quasi-spherical limit via mismatches and present one phasing comparison against a precessing, eccentric simulation from the RIT catalog.