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Periastron advance in spinning black hole binaries: comparing effective-one-body and numerical relativity

Hinderer, Tanja and Buonanno, Alessandra and Mroué, Abdul H. and Hemberger, Daniel A. and Lovelace, Geoffrey and Pfeiffer, Harald P. and Kidder, Lawrence E. and Scheel, Mark A. and Szilágyi, Béla and Taylor, Nicholas W. and Teukolsky, Saul A. (2013) Periastron advance in spinning black hole binaries: comparing effective-one-body and numerical relativity. Physical Review D, 88 (8). Art. No. 084005. ISSN 2470-0010. https://resolver.caltech.edu/CaltechAUTHORS:20131113-094821753

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Abstract

We compute the periastron advance using the effective-one-body formalism for binary black holes moving on quasicircular orbits and having spins collinear with the orbital angular momentum. We compare the predictions with the periastron advance recently computed in accurate numerical-relativity simulations and find remarkable agreement for a wide range of spins and mass ratios. These results do not use any numerical-relativity calibration of the effective-one-body model, and stem from two key ingredients in the effective-one-body Hamiltonian: (i) the mapping of the two-body dynamics of spinning particles onto the dynamics of an effective spinning particle in a (deformed) Kerr spacetime, fully symmetrized with respect to the two-body masses and spins, and (ii) the resummation, in the test-particle limit, of all post-Newtonian corrections linear in the spin of the particle. In fact, even when only the leading spin post-Newtonian corrections are included in the effective-one-body spinning Hamiltonian but all the test-particle corrections linear in the spin of the particle are resummed we find very good agreement with the numerical results (within the numerical error for equal-mass binaries and discrepancies of at most 1% for larger mass ratios). Furthermore, we specialize to the extreme mass-ratio limit and derive, using the equations of motion in the gravitational skeleton approach, analytical expressions for the periastron advance, the meridional Lense-Thirring precession and spin precession frequency in the case of a spinning particle on a nearly circular equatorial orbit in Kerr spacetime, including also terms quadratic in the spin.


Item Type:Article
Related URLs:
URLURL TypeDescription
http://dx.doi.org/10.1103/PhysRevD.88.084005DOIArticle
http://link.aps.org/doi/10.1103/PhysRevD.88.084005PublisherArticle
http://arxiv.org/abs/1309.0544arXivDiscussion Paper
ORCID:
AuthorORCID
Hinderer, Tanja0000-0002-3394-6105
Lovelace, Geoffrey0000-0002-7084-1070
Pfeiffer, Harald P.0000-0001-9288-519X
Kidder, Lawrence E.0000-0001-5392-7342
Teukolsky, Saul A.0000-0001-9765-4526
Additional Information:© 2013 American Physical Society. Received 3 September 2013; published 4 October 2013. We thank Andrea Taracchini and Yi Pan for help with implementing the EOB Hamiltonian and Enrico Barausse, Alexandre Le Tiec, Yi Pan and Andrea Taracchini for useful interactions and comments. A. B. acknowledges partial support from NSF Grants No. PHY-0903631 and No. PHY-1208881, and NASA Grant No. NNX09AI81G. T. H. acknowledges support from NSF Grants No. PHY-0903631 and No. PHY-1208881 and 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. We acknowledge support from the Sherman Fairchild Foundation, from NSF Grants No. PHY-0969111 and No. PHYS-1005426 at Cornell, and from NSF Grants No. PHY-1068881 and No. PHY- 1005655 at Caltech. The numerical-relativity simulations were performed at the GPC supercomputer at the SciNet HPC Consortium [95]; 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 is 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.
Funders:
Funding AgencyGrant Number
NSFPHY-0903631
NSFPHY-1208881
NASANNX09AI81G
NSFPHY-0903631
NSFPHY-1208881
Maryland Center for Fundamental PhysicsUNSPECIFIED
NSERC (Canada)UNSPECIFIED
Canada Research Chairs ProgramUNSPECIFIED
Canadian Institute for Advanced Research (CIAR)UNSPECIFIED
Sherman Fairchild FoundationUNSPECIFIED
NSFPHY-0969111
NSFPHYS-1005426
NSFPHY-1068881
NSFPHY-1005655
NSF MRI-R2PHY-0960291
NSF XSEDE networkTG-PHY990007N
Canada Foundation for Innovation (CFI)UNSPECIFIED
Compute CanadaUNSPECIFIED
Government of OntarioUNSPECIFIED
Ontario Research Fund-Research ExcellenceUNSPECIFIED
University of TorontoUNSPECIFIED
Issue or Number:8
Classification Code:PACS: 04.30.-w, 04.25.-g
Record Number:CaltechAUTHORS:20131113-094821753
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20131113-094821753
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:42416
Collection:CaltechAUTHORS
Deposited By: Jason Perez
Deposited On:13 Nov 2013 21:36
Last Modified:09 Mar 2020 13:19

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