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Comparing post-Newtonian and numerical relativity precession dynamics

Ossokine, Serguei and Boyle, Michael and Kidder, Lawrence E. and Pfeiffer, Harald P. and Scheel, Mark A. and Szilágyi, Béla (2015) Comparing post-Newtonian and numerical relativity precession dynamics. Physical Review D, 92 (10). Art. No. 104028. ISSN 1550-7998.

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Binary black-hole systems are expected to be important sources of gravitational waves for upcoming gravitational-wave detectors. If the spins are not colinear with each other or with the orbital angular momentum, these systems exhibit complicated precession dynamics that are imprinted on the gravitational waveform. We develop a new procedure to match the precession dynamics computed by post-Newtonian (PN) theory to those of numerical binary black-hole simulations in full general relativity. For numerical relativity (NR) simulations lasting approximately two precession cycles, we find that the PN and NR predictions for the directions of the orbital angular momentum and the spins agree to better than ∼1° with NR during the inspiral, increasing to 5° near merger. Nutation of the orbital plane on the orbital time scale agrees well between NR and PN, whereas nutation of the spin direction shows qualitatively different behavior in PN and NR. We also examine how the PN equations for precession and orbital-phase evolution converge with PN order, and we quantify the impact of various choices for handling partially known PN terms.

Item Type:Article
Related URLs:
URLURL TypeDescription Paper
Kidder, Lawrence E.0000-0001-5392-7342
Pfeiffer, Harald P.0000-0001-9288-519X
Additional Information:© 2015 American Physical Society. Received 5 February 2015; published 9 November 2015. We thank Kipp Cannon, Francois Foucart, Prayush Kumar, Abdul Mroué and Aaron Zimmerman for useful discussions. Calculations were performed with the SpEC code [73].We gratefully acknowledge support from NSERC of Canada, from the Canada Research Chairs Program, and from the Canadian Institute for Advanced Research. We further gratefully acknowledge support from the Sherman Fairchild Foundation, from National Science Foundation Grants No. PHY-1306125 and No.AST-1333129 at Cornell, and from National Science Foundation Grants No. PHY- 1440083, No. AST-1333520, and No. PHY-1404569 at Caltech. Calculations were performed at the GPC supercomputer at the SciNet HPC Consortium [74]. SciNet is funded by the Canada Foundation for Innovation (CFI) under the auspices of Compute Canada, the Government of Ontario, Ontario Research Fund (ORF)—Research Excellence, and the University of Toronto. Further computations were performed on the Zwicky cluster at Caltech, which is supported by the Sherman Fairchild Foundation and by National Science Foundation Award No. PHY-0960291, and on the National Science Foundation XSEDE network under Grant No. TG-PHY990007N.
Funding AgencyGrant Number
Natural Sciences and Engineering Research Council of Canada (NSERC)UNSPECIFIED
Canada Research Chairs ProgramUNSPECIFIED
Canadian Institute for Advanced ResearchUNSPECIFIED
Sherman Fairchild FoundationUNSPECIFIED
Canada Foundation for Innovation (CFI)UNSPECIFIED
Government of OntarioUNSPECIFIED
Ontario Research Fund-Research ExcellenceUNSPECIFIED
University of TorontoUNSPECIFIED
Issue or Number:10
Classification Code:PACS numbers: 04.25.D-, 04.25.dg, 04.25.Nx
Record Number:CaltechAUTHORS:20151207-111830327
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Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:62653
Deposited By: Tony Diaz
Deposited On:08 Dec 2015 17:05
Last Modified:09 Mar 2020 13:19

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