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

Buonanno, A., Pan, Y., Baker, J. G., Centrella, J., Kelly, B. J., McWilliams, S. T., et al. (2007). Toward faithful templates for non-spinning binary black holes using the effective-one-body approach. Physical Review D, 76: 104049. doi:10.1103/PhysRevD.76.104049.

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Item Permalink: http://hdl.handle.net/11858/00-001M-0000-0018-C5E1-8 Version Permalink: http://hdl.handle.net/11858/00-001M-0000-0018-C5E3-4
Genre: Journal Article

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 Creators:
Buonanno, Alessandra1, 2, Author              
Pan, Yi, Author
Baker, John G., Author
Centrella, Joan, Author
Kelly, Bernard J., Author
McWilliams, Sean T., Author
van Meter, James R., Author
Affiliations:
1Maryland Center for Fundamental Physics, Department of Physics, University of Maryland, ou_persistent22              
2Astrophysical and Cosmological Relativity, AEI-Golm, MPI for Gravitational Physics, Max Planck Society, ou_1933290              

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Free keywords: General Relativity and Quantum Cosmology, gr-qc
 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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 Dates: 2007-06-252008-01-042007
 Publication Status: Published in print
 Pages: 15 pages, 9 figures
 Publishing info: -
 Table of Contents: -
 Rev. Method: -
 Identifiers: arXiv: 0706.3732
DOI: 10.1103/PhysRevD.76.104049
URI: http://arxiv.org/abs/0706.3732
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Title: Physical Review D
  Other : Phys. Rev. D.
Source Genre: Journal
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Publ. Info: Lancaster, Pa. : American Physical Society
Pages: - Volume / Issue: 76 Sequence Number: 104049 Start / End Page: - Identifier: ISSN: 0556-2821
CoNE: /journals/resource/111088197762258