Researchers have developed SEOBNRv6EHM, a new gravitational wave model that accurately simulates the emission from binary black hole (BBH) systems in generic planar orbits. This model is crucial for gravitational wave astronomy, as it allows for the inference of compact binary parameters, including orbital eccentricity, a key indicator of dynamic formation channels. Eccentricity is a fundamental parameter that, if not accounted for, can introduce systematic errors in gravitational wave analyses.

The SEOBNRv6EHM model is based on the Effective-One-Body (EOB) formalism and has been calibrated using numerical relativity (NR) simulations from the SXS collaboration for quasi-circular orbits. In addition to the dominant (2,2) mode, the model includes multipoles such as (2,1), (3,3), (3,2), (4,4), and (4,3), covering the complete inspiral, merger, and ringdown process of coalescing binaries, as well as dynamic captures and scattering encounters. The novelty lies in the application of new resummations of the radiation reaction force and wave modes.

The accuracy of SEOBNRv6EHM has been validated through extensive comparisons with 592 NR simulations of quasi-circular systems, 319 of eccentric systems, one dynamic capture, and two scattering events from SXS. For highly eccentric systems, the model achieves unprecedented accuracy, with waveform mismatches below or close to 2% across a total mass range of 20 to 200 M☉ and eccentricities up to ~0.9 in the 14 periastron passages prior to merger. Furthermore, SEOBNRv6EHM is significantly faster, generating waveforms 2 to 6 times faster than other advanced eccentric EOB models, making it ideal for applications in gravitational wave astronomy.