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Adding eccentricity to quasicircular binary-black-hole waveform models
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abstract
The detection of gravitational-wave signals from coalescing eccentric binary black holes would yield unprecedented information about the formation and evolution of compact binaries in specific scenarios, such as dynamical formation in dense stellar clusters and three-body interactions. The gravitational-wave searches by the ground-based interferometers, LIGO and Virgo, rely on analytical waveform models for binaries on quasicircular orbits. Eccentric merger waveform models are less developed, and only few numerical simulations of eccentric mergers are publicly available, but several eccentric inspiral models have been developed from the post-Newtonian expansion. Here we present a novel method to convert the dominant quadrupolar mode of any circular analytical binary-black-hole model into an eccentric model. First, using numerical simulations, we examine the additional amplitude and frequency modulations of eccentric signals that are not present in their circular counterparts. Subsequently, we identify suitable analytical descriptions of those modulations and interpolate key parameters from twelve numerical simulations designated as our training dataset. This allows us to reconstruct the modulated amplitude and phase of any waveform up to mass ratio 3 and eccentricity 0.2. We find that the minimum overlap of the new model with numerical simulations is around 0.98 over all of our test dataset that are scaled to a 50M$_\odot$ black-hole binary starting at 35 Hz with aLIGO A+ design sensitivity. A Python package \pyrex easily carries out the computation of this method.
Forward citations
Cited by 7 Pith papers
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Third post-Newtonian dynamics for eccentric orbits and aligned spins in the effective-one-body waveform model SEOBNRv5EHM
The authors obtain, for the first time, 3PN-accurate eccentric-orbit fluxes, radiation-reaction force, and waveform modes in the effective-one-body formalism, and use them to build the SEOBNRv5EHM inspiral model.
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Accurate waveforms for eccentric, aligned-spin binary black holes: The multipolar effective-one-body model SEOBNRv5EHM
SEOBNRv5EHM, a new effective-one-body waveform model with third-post-Newtonian eccentricity corrections, reaches a median 0.02% mismatch against eccentric numerical-relativity simulations, about an order of magnitude ...
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A geometric template bank for the detection of spinning low-mass compact binaries with moderate orbital eccentricity
A geometric template bank including eccentricity recovers moderately eccentric BNS/NSBH signals with less than 6% loss, while quasi-circular banks miss up to 40%.
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Chase Orbits, not Time: A Scalable Paradigm for Long-Duration Eccentric Gravitational-Wave Surrogates
Eccentric inspiral waveforms are modeled against mean anomaly rather than time, yielding an order-of-magnitude compression and a 2.77e6 M surrogate that is ~20x faster to evaluate.
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Data-driven extraction, phenomenology and modeling of eccentric harmonics in binary black hole merger waveforms
Eccentric merger waveforms decompose into four smooth harmonics whose phases follow j times a common orbital phase plus an eccentricity-only correction, and whose mean-anomaly dependence can be fitted with simple functions.
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gwharmone: first data-driven surrogate for eccentric harmonics in binary black hole merger waveforms
gwharmone is a data-driven surrogate that reproduces the eccentric harmonics of the dominant quadrupole mode in non-spinning eccentric binary black hole waveforms with average frequency-domain mismatches near 0.004.
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Post-Newtonian theory-inspired framework for characterizing eccentricity in gravitational waveforms
A PN-anchored waveform-based eccentricity estimator using envelope fits to the universal eccentric modulation, with an empirically added half-PN term.
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