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Journal Article

Inspiral-Merger-Ringdown Waveforms for Black-Hole Binaries with Nonprecessing Spins

MPS-Authors

Ajith,  P.
Observational Relativity and Cosmology, AEI-Hannover, MPI for Gravitational Physics, Max Planck Society;

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Husa,  Sascha
Astrophysical Relativity, AEI-Golm, MPI for Gravitational Physics, Max Planck Society;

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Chen,  Yanbei
Astrophysical Relativity, AEI-Golm, MPI for Gravitational Physics, Max Planck Society;

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Dorband,  Nils
Astrophysical Relativity, AEI-Golm, MPI for Gravitational Physics, Max Planck Society;

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Ohme,  Frank
Astrophysical Relativity, AEI-Golm, MPI for Gravitational Physics, Max Planck Society;

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Pollney,  Denis
Astrophysical Relativity, AEI-Golm, MPI for Gravitational Physics, Max Planck Society;

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Reisswig,  Christian
Astrophysical Relativity, AEI-Golm, MPI for Gravitational Physics, Max Planck Society;

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Santamaria,  Lucia
Astrophysical Relativity, AEI-Golm, MPI for Gravitational Physics, Max Planck Society;

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Seiler,  Jennifer
Astrophysical Relativity, AEI-Golm, MPI for Gravitational Physics, Max Planck Society;

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Fulltext (public)

0909.2867
(Preprint), 781KB

PRLe241101.pdf
(Any fulltext), 366KB

0909.2867v3.pdf
(Preprint), 268KB

Supplementary Material (public)
There is no public supplementary material available
Citation

Ajith, P., Hannam, M., Husa, S., Chen, Y., Bruegmann, B., Dorband, N., et al. (2011). Inspiral-Merger-Ringdown Waveforms for Black-Hole Binaries with Nonprecessing Spins. Pysical Review Letters, 106: 241101. doi:10.1103/PhysRevLett.106.241101.


Cite as: http://hdl.handle.net/11858/00-001M-0000-0012-9C95-2
Abstract
We present the first analytical inspiral-merger-ringdown gravitational waveforms from black-hole (BH) binaries with non-precessing spins. By matching a post-Newtonian description of the inspiral to a set of numerical calculations performed in full general relativity, we obtain a waveform family with a conveniently small number of physical parameters. The physical content of these waveforms includes the "orbital hang-up" effect, when BHs are spinning rapidly along the direction of the orbital angular momentum. These waveforms will allow us to detect a larger parameter space of BH binary coalescence, to explore various scientific questions related to GW astronomy, and could dramatically improve the expected detection rates of GW detectors.