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Improved inspiral-merger-ringdown model for BBHs on elliptical orbits
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abstract
Gravitational waveforms capturing binary evolution through the early-inspiral phase play a critical role in extracting orbital features that nearly disappear during the late-inspiral and subsequent merger phase due to radiation reaction forces; for instance, the effect of orbital eccentricity. Phenomenological approaches that model compact binary mergers rely heavily on combining inputs from both analytical and numerical approaches to reduce the computational cost of generating templates for data analysis purposes. In a recent work, Chattaraj et al., Phys. Rev. D 106, 124008 (2022) constructed a dominant ($\ell=2$, $|m|=2$) mode model for nonspinning binary black holes (BBHs) on elliptical orbits. The model was constructed in time domain and is fully analytical. The current work is an attempt to improve this model by making a few important changes in our approach. The most significant of those involves identifying initial values of orbital parameters with which the inspiral part of the model is evolved. While the ingredients remain the same as in the previous work, the resulting (new) model, when compared against a set of target waveforms constructed here, produces match values better than 96.5% for systems heavier than $80M_\odot$, while with the old model this limit on the total mass is $115M_\odot$. The updated model is validated against an independent eccentric waveform family (TEOBResumS-Dali) for an initial eccentricity ($e_0$), mass ratio ($q$) and mean anomaly ($l_0$) in the range $0\lesssim e_0\lesssim0.3$, $1\lesssim q\lesssim3$ and $-\pi\leq l_0\leq\pi$, respectively. Further, an alternate model including the effect of higher order modes is also provided. Finally, while our model assumes nonspinning components, we show that it could also be used for systems with component spin vectors (anti-) aligned w.r.t. the orbital angular momentum and small spin magnitudes.
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
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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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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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Spin effects in the phasing formula of eccentric compact binary inspirals up to the third post-Newtonian order
Closed-form post-Newtonian phasing formulas for eccentric, spin-aligned compact binary inspirals are derived to 3PN order and to eighth order in initial eccentricity, with a resummation extending validity to e0 around 0.55.
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