SEOBNRv6EHM is a multipolar EOB model for eccentric planar-orbit BBHs calibrated to NR simulations, showing low waveform mismatches up to eccentricity 0.9.
Efficient gravitational-wave model for fully-precessing and moderately eccentric, compact binary inspirals
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pyEFPEHM extends prior PN models to include higher-order quasi-circular phasing, generalized precession solutions, and eccentric corrections up to 1PN in selected multipoles for eccentric precessing binaries with matter effects.
An analytical 2PN solution is constructed for the orbital and spin dynamics of eccentric, arbitrarily spinning binary black holes, with spin oscillations retained only at 1.5PN accuracy.
A framework using scale separation in the Isaacson description defines observable gravitational memory rise for compact binary coalescences, providing a basis for hypothesis testing in LISA data.
Eccentricity-induced higher harmonics allow binary neutron star gravitational wave signals to reach detection thresholds and achieve useful localization several minutes earlier in 2G detector networks than circular signals.
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Enhancing Early Detection and Localization of Gravitational Waves via Eccentricity-Induced Higher Harmonic Modes with 2G Detector Networks
Eccentricity-induced higher harmonics allow binary neutron star gravitational wave signals to reach detection thresholds and achieve useful localization several minutes earlier in 2G detector networks than circular signals.