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arXiv · 0706.3732

Toward faithful templates for non-spinning binary black holes using the effective-one-body approach

Alessandra Buonanno·Yi Pan·John G. Baker·Joan Centrella·Bernard J. Kelly·Sean T. McWilliams·James R. van Meter
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Abstract

We present an accurate approximation of the full gravitational radiation waveforms generated in the merger of non-eccentric systems of two non-spinning black holes. Utilizing information from recent numerical relativity simulations and the natural flexibility of the effective-one-body (EOB) model, we extend the latter so that it can successfully match the numerical relativity waveforms during the last stages of inspiral, merger and ringdown. By ``successfully'' here, we mean with phase differences < 8% of a gravitational-wave cycle accumulated by the end of the ringdown phase, maximizing only over time of arrival and initial phase. We obtain this result by simply adding a 4-post-Newtonian order correction in the EOB radial potential and determining the (constant) coefficient by imposing high-matching performances with numerical waveforms of mass ratios m1/m2 = 1, 3/2, 2 and 4, m1 and m2 being the individual black-hole masses. The final black-hole mass and spin predicted by the numerical simulations are used to determine the ringdown frequency and decay time of three quasi-normal-mode damped sinusoids that are attached to the EOB inspiral-(plunge) waveform at the EOB light-ring. The EOB waveforms might be tested and further improved in the future by comparison with extremely long and accurate inspiral numerical-relativity waveforms. They may already be employed for coherent searches and parameter estimation of gravitational waves emitted by non-spinning coalescing binary black holes with ground-based laser-interferometer detectors.

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Alessandra Buonanno, Yi Pan, John G. Baker, Joan Centrella, Bernard J. Kelly, Sean T. McWilliams, James R. van Meter. 2008-01-04. Toward faithful templates for non-spinning binary black holes using the effective-one-body approach. https://doi.org/10.1103/physrevd.76.104049

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