For orbital velocities below 0.45, PN energy flux agreement with NR improves up to incomplete 6PN with non-monotonic behavior, but convergence is lost near v approximately 0.5.
SpECTRE Cauchy-characteristic evolution system for rapid, precise waveform extraction
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Two new surrogate models, trained on NR simulations, predict remnant properties and eccentricity dynamics for nonspinning eccentric black hole binaries with q ≤ 4 and e < 0.23.
Hierarchical Bayesian inference on GWTC-5.0 constrains the memory enhancement factor to 0.26 with large uncertainties consistent with the GR value of 1 and forecasts that 2000 detections are needed for a 1σ constraint away from zero.
Quadratic quasinormal modes and the memory effect in black hole ringdown are related through bridge coefficients that depend primarily on remnant black hole parameters.
citing papers explorer
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Convergence of post-Newtonian for quasi-circular non-precessing comparable mass ratios BBHs
For orbital velocities below 0.45, PN energy flux agreement with NR improves up to incomplete 6PN with non-monotonic behavior, but convergence is lost near v approximately 0.5.
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Merger remnant and eccentricity dynamics surrogates for eccentric nonspinning black hole binaries
Two new surrogate models, trained on NR simulations, predict remnant properties and eccentricity dynamics for nonspinning eccentric black hole binaries with q ≤ 4 and e < 0.23.
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Constraining Gravitational Wave Memory with Hierarchical Inference
Hierarchical Bayesian inference on GWTC-5.0 constrains the memory enhancement factor to 0.26 with large uncertainties consistent with the GR value of 1 and forecasts that 2000 detections are needed for a 1σ constraint away from zero.
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Can Oscillatory and Persistent Nonlinearities Be Bridged in Black Hole Ringdown?
Quadratic quasinormal modes and the memory effect in black hole ringdown are related through bridge coefficients that depend primarily on remnant black hole parameters.