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Comparing gravitational waveform extrapolation to Cauchy-characteristic extraction in binary black hole simulations

Taylor, Nicholas W. and Boyle, Michael and Reisswig, Christian and Scheel, Mark A. and Chu, Tony and Kidder, Lawrence E. and Szilágyi, Béla (2013) Comparing gravitational waveform extrapolation to Cauchy-characteristic extraction in binary black hole simulations. Physical Review D, 88 (12). Art. No. 124010. ISSN 2470-0010. doi:10.1103/PhysRevD.88.124010.

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We extract gravitational waveforms from numerical simulations of black hole binaries computed using the Spectral Einstein Code. We compare two extraction methods: direct construction of the Newman-Penrose (NP) scalar Ψ_4 at a finite distance from the source and Cauchy-characteristic extraction (CCE). The direct NP approach is simpler than CCE, but NP waveforms can be contaminated by near-zone effects—unless the waves are extracted at several distances from the source and extrapolated to infinity. Even then, the resulting waveforms can in principle be contaminated by gauge effects. In contrast, CCE directly provides, by construction, gauge-invariant waveforms at future null infinity. We verify the gauge invariance of CCE by running the same physical simulation using two different gauge conditions. We find that these two gauge conditions produce the same CCE waveforms but show differences in extrapolated-Ψ_4 waveforms. We examine data from several different binary configurations and measure the dominant sources of error in the extrapolated-Ψ4 and CCE waveforms. In some cases, we find that NP waveforms extrapolated to infinity agree with the corresponding CCE waveforms to within the estimated error bars. However, we find that in other cases extrapolated and CCE waveforms disagree, most notably for m=0 “memory” modes.

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Kidder, Lawrence E.0000-0001-5392-7342
Additional Information:© 2013 American Physical Society. Received 13 September 2013; published 3 December 2013. We thank Nigel Bishop, Ian Hinder, Lee Lindblom, Harald Pfeiffer, and Jeffrey Winicour for helpful discussions. We thank Christian Ott for help in initiating and completing this project. We gratefully acknowledge support from the Sherman Fairchild Foundation; from NSF Grants No. PHY-1068881, No. PHY-1005655, and No. DMS-1065438 at Caltech; and from NSF Grants No. PHY-0969111 and No. PHY-1005426, and NASA Grant No. NNX09AF96G at Cornell. C. R. acknowledges support by NASA through Einstein Postdoctoral Fellowship Grant No. PF2-130099 awarded by the Chandra X-ray Center, which is operated by the Smithsonian Astrophysical Observatory for NASA under Contract No. NAS8-03060. Simulations used in this work were computed with SpEC [13]. Computations were performed on the Zwicky cluster at Caltech, which is supported by the Sherman Fairchild Foundation and by NSF Award PHY-0960291; on the NSF XSEDE network under Grant No. TG-PHY990007N; and on the GPC supercomputer at the SciNet HPC Consortium [99]. SciNet is funded by the Canada Foundation for Innovation under the auspices of Compute Canada, the Government of Ontario, Ontario Research Fund–Research Excellence, and the University of Toronto.
Funding AgencyGrant Number
Sherman Fairchild FoundationUNSPECIFIED
NASA Einstein Postdoctoral FellowshipPF2-130099
Canada Foundation for Innovation (CFI)UNSPECIFIED
Government of OntarioUNSPECIFIED
Ontario Research Fund–Research ExcellenceUNSPECIFIED
University of TorontoUNSPECIFIED
Issue or Number:12
Classification Code: PACS: 04.25.D-, 02.70.Hm, 04.25.dg, 04.30.-w
Record Number:CaltechAUTHORS:20140122-092930548
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Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:43463
Deposited On:23 Jan 2014 21:24
Last Modified:10 Nov 2021 16:38

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