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  High accuracy binary black hole simulations with an extended wave zone

Pollney, D., Reisswig, C., Schnetter, E., Dorband, N., & Diener, P. (2011). High accuracy binary black hole simulations with an extended wave zone. Physical Review D, 83(4): 044045. doi:10.1103/PhysRevD.83.044045.

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Datensatz-Permalink: http://hdl.handle.net/11858/00-001M-0000-000F-104E-3 Versions-Permalink: http://hdl.handle.net/11858/00-001M-0000-000F-104F-1
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 Urheber:
Pollney, Denis1, Autor              
Reisswig, Christian1, Autor              
Schnetter, Erik, Autor
Dorband, Nils1, Autor              
Diener, Peter, Autor
Affiliations:
1Astrophysical Relativity, AEI-Golm, MPI for Gravitational Physics, Max Planck Society, ou_24013              

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Schlagwörter: General Relativity and Quantum Cosmology, gr-qc
 Zusammenfassung: We present results from a new code for binary black hole evolutions using the moving-puncture approach, implementing finite differences in generalised coordinates, and allowing the spacetime to be covered with multiple communicating non-singular coordinate patches. Here we consider a regular Cartesian near zone, with adapted spherical grids covering the wave zone. The efficiencies resulting from the use of adapted coordinates allow us to maintain sufficient grid resolution to an artificial outer boundary location which is causally disconnected from the measurement. For the well-studied test-case of the inspiral of an equal-mass non-spinning binary (evolved for more than 8 orbits before merger), we determine the phase and amplitude to numerical accuracies better than 0.010% and 0.090% during inspiral, respectively, and 0.003% and 0.153% during merger. The waveforms, including the resolved higher harmonics, are convergent and can be consistently extrapolated to $r\to\infty$ throughout the simulation, including the merger and ringdown. Ringdown frequencies for these modes (to $(\ell,m)=(6,6)$) match perturbative calculations to within 0.01%, providing a strong confirmation that the remnant settles to a Kerr black hole with irreducible mass $M_{\rm irr} = 0.884355\pm20\times10^{-6}$ and spin $S_f/M_f^2 = 0.686923 \pm 10\times10^{-6}$

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 Datum: 2009-10-202011
 Publikationsstatus: Im Druck veröffentlicht
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 Identifikatoren: arXiv: 0910.3803
DOI: 10.1103/PhysRevD.83.044045
URI: http://arxiv.org/abs/0910.3803
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Titel: Physical Review D
  Andere : Phys. Rev. D.
Genre der Quelle: Zeitschrift
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Affiliations:
Ort, Verlag, Ausgabe: Lancaster, Pa. : Published for the American Physical Society by the American Institute of Physics
Seiten: - Band / Heft: 83 (4) Artikelnummer: 044045 Start- / Endseite: - Identifikator: ISSN: 0556-2821
CoNE: /journals/resource/111088197762258