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Periastron advance in spinning black hole binaries: Gravitational self-force from numerical relativity

Le Tiec, Alexandre and Buonanno, Alessandra and Mroué, Abdul H. and Pfeiffer, Harald P. and Hemberger, Daniel A. and Lovelace, Geoffrey and Kidder, Lawrence E. and Scheel, Mark A. and Szilágyi, Bela and Taylor, Nicholas W. and Teukolsky, Saul A. (2013) Periastron advance in spinning black hole binaries: Gravitational self-force from numerical relativity. Physical Review D, 88 (12). Art. No. 124027. ISSN 2470-0010.

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We study the general relativistic periastron advance in spinning black hole binaries on quasicircular orbits, with spins aligned or antialigned with the orbital angular momentum, using numerical-relativity simulations, the post-Newtonian approximation, and black hole perturbation theory. By imposing a symmetry by exchange of the bodies’ labels, we devise an improved version of the perturbative result and use it as the leading term of a new type of expansion in powers of the symmetric mass ratio. This allows us to measure, for the first time, the gravitational self-force effect on the periastron advance of a nonspinning particle orbiting a Kerr black hole of mass M and spin S=−0.5M^2, down to separations of order 9M. Comparing the predictions of our improved perturbative expansion with the exact results from numerical simulations of equal-mass and equal-spin binaries, we find a remarkable agreement over a wide range of spins and orbital separations.

Item Type:Article
Related URLs:
URLURL TypeDescription Paper
Pfeiffer, Harald P.0000-0001-9288-519X
Lovelace, Geoffrey0000-0002-7084-1070
Kidder, Lawrence E.0000-0001-5392-7342
Teukolsky, Saul A.0000-0001-9765-4526
Additional Information:© 2013 American Physical Society. Received 2 September 2013; published 9 December 2013. A. B. and A. L. T. acknowledge support from NSF through Grants No. PHY-0903631 and No. PHY-1208881. A. B. also acknowledges support from NASA through Grant No. NNX09AI81G and A. L. T. from the Maryland Center for Fundamental Physics. A. M. and H. P. acknowledge support from NSERC of Canada, from the Canada Research Chairs Program, and from the Canadian Institute for Advanced Research. D. H., L. K., G. L., and S. T. acknowledge support from the Sherman Fairchild Foundation and NSF Grants No. PHY-1306125 and No. PHYS-1005426 at Cornell. M. S., B. S., and N. T. gratefully acknowledge support from the Sherman Fairchild Foundation and NSF Grants No. PHY-1068881, No. PHY-1005655, and No. DMS-1065438 at Caltech. The numerical relativity simulations were performed at the GPC supercomputer at the SciNet HPC Consortium [65]; SciNet is funded by the Canada Foundation for Innovation (CFI) under the auspices of Compute Canada; the Government of Ontario; Ontario Research Fund–Research Excellence; and the University of Toronto. Further computations were performed on the Caltech computer cluster Zwicky, which was funded by the Sherman Fairchild Foundation and the NSF MRI-R2 Grant No. PHY- 0960291, on SHC at Caltech, which is supported by the Sherman Fairchild Foundation, and on the NSF XSEDE network under Grant No. TG-PHY990007N.
Funding AgencyGrant Number
Canada Research Chairs ProgramUNSPECIFIED
Canadian Institute for Advanced ResearchUNSPECIFIED
Sherman Fairchild FoundationUNSPECIFIED
Maryland Center for Fundamental PhysicsUNSPECIFIED
NSF MRI-R2PHY-0960291
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-, 04.25.dg, 04.25.Nx, 04.30.-w
Record Number:CaltechAUTHORS:20140116-093422080
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Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:43401
Deposited By: Jason Perez
Deposited On:16 Jan 2014 23:26
Last Modified:09 Mar 2020 13:19

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