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  Prototype effective-one-body model for nonprecessing spinning inspiral-merger-ringdown waveforms

Taracchini, A., Pan, Y., Buonanno, A., Barausse, E., Boyle, M., Chu, T., et al. (2012). Prototype effective-one-body model for nonprecessing spinning inspiral-merger-ringdown waveforms. Physical Review D, 86(2): 024011. doi:10.1103/PhysRevD.86.024011.

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 Creators:
Taracchini, Andrea, Author
Pan, Yi, Author
Buonanno, A.1, 2, Author           
Barausse, Enrico, Author
Boyle, Michael, Author
Chu, Tony, Author
Lovelace, Geoffrey, Author
Pfeiffer, Harald P., Author
Scheel, Mark A., Author
Affiliations:
1Astrophysical and Cosmological Relativity, AEI-Golm, MPI for Gravitational Physics, Max Planck Society, ou_1933290              
2Maryland Center for Fundamental Physics & Joint Space-Science Center, Department of Physics, University of Maryland, ou_persistent22              

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Free keywords: General Relativity and Quantum Cosmology, gr-qc
 Abstract: We first use five non-spinning and two mildly spinning (chi_i \simeq -0.44, +0.44) numerical-relativity waveforms of black-hole binaries and calibrate an effective-one-body (EOB) model for non-precessing spinning binaries, notably its dynamics and the dominant (2,2) gravitational-wave mode. Then, we combine the above results with recent outcomes of small-mass-ratio simulations produced by the Teukolsky equation and build a prototype EOB model for detection purposes, which is capable of generating inspiral-merger-ringdown waveforms for non-precessing spinning black-hole binaries with any mass ratio and individual black-hole spins -1 \leq chi_i \lesssim 0.7. We compare the prototype EOB model to two equal-mass highly spinning numerical-relativity waveforms of black holes with spins chi_i = -0.95, +0.97, which were not available at the time the EOB model was calibrated. In the case of Advanced LIGO we find that the mismatch between prototype-EOB and numerical-relativity waveforms is always smaller than 0.003 for total mass 20-200 M_\odot, the mismatch being computed by maximizing only over the initial phase and time. To successfully generate merger waveforms for individual black-hole spins chi_i \gtrsim 0.7, the prototype-EOB model needs to be improved by (i) better modeling the plunge dynamics and (ii) including higher-order PN spin terms in the gravitational-wave modes and radiation-reaction force.

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 Dates: 2012-02-032012-08-212012
 Publication Status: Issued
 Pages: 20 pages, 8 figures. Minor changes to match version accepted for publication in PRD
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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: 86 (2) Sequence Number: 024011 Start / End Page: - Identifier: ISSN: 0556-2821
CoNE: https://pure.mpg.de/cone/journals/resource/111088197762258