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Collisions of oppositely charged black holes

Zilhão, Miguel and Cardoso, Vitor and Herdeiro, Carlos and Lehner, Luis and Sperhake, Ulrich (2014) Collisions of oppositely charged black holes. Physical Review D, 89 (4). Art. No. 044008. ISSN 2470-0010. doi:10.1103/PhysRevD.89.044008.

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The first fully nonlinear numerical simulations of colliding charged black holes in D=4 Einstein-Maxwell theory were recently reported [Zilhão et al., Phys. Rev. D 85, 124062 (2012)]. These collisions were performed for black holes with equal charge-to-mass ratio, for which initial data can be found in closed analytic form. Here we generalize the study of collisions of charged black holes to the case of unequal charge-to-mass ratios. We focus on oppositely charged black holes, as to maximize acceleration-dependent effects. As |Q|/M increases from 0 to 0.99, we observe that the gravitational radiation emitted increases by a factor of ∼2.7; the electromagnetic radiation emission becomes dominant for |Q|/M≳0.37 and at |Q|/M=0.99 is larger, by a factor of ∼5.8, than its gravitational counterpart. We observe that these numerical results exhibit a precise and simple scaling with the charge. Furthermore, we show that the results from the numerical simulations are qualitatively captured by a simple analytic model that computes the electromagnetic dipolar radiation and the gravitational quadrupolar radiation of two nonrelativistic interacting particles in Minkowski spacetime.

Item Type:Article
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Sperhake, Ulrich0000-0002-3134-7088
Additional Information:© 2014 American Physical Society. Received 3 December 2013; published 11 February 2014. We thank J. C. Degollado for helpful discussions. M. Z. is supported by NSF Grants No. OCI-0832606, No. PHY- 0969855, No. AST-1028087, and No. PHY-1229173. V. C. acknowledges financial support provided under the European Union’s FP7 ERC Starting Grant “The dynamics of black holes: testing the limits of Einstein’s theory” Grant Agreement No. DyBHo-256667. U. S. acknowledges support by the FP7-PEOPLE-2011-CIG CBHEO Grant No. 293412, the STFC Grant No. ST/I002006/1, the XSEDE Grant No. PHY-090003 by the National Science Foundation, the COSMOS supercomputer infrastructure, part of the DiRAC HPC Facility funded by STFC and BIS, and the Centro de Supercomputacion de Galicia (CESGA) under Grant No. ICTS-2013-249, This research was supported in part by Perimeter Institute for Theoretical Physics. Research at Perimeter Institute is supported by the Government of Canada through Industry Canada and by the Province of Ontario through the Ministry of Economic Development & Innovation. This work was supported by the NRHEP 295189 FP7-PEOPLE-2011-IRSES Grant, and by FCT-Portugal through Projects No. PTDC/FIS/116625/ 2010 and No. CERN/FP/123593/2011. Computations were performed on the “Baltasar Sete-Sois” cluster at IST, the “Blafis” cluster at Universidade deAveiro, the NICS Kraken Cluster, the SDSC Trestles Cluster, Cambridge’s COSMOS, on the “venus” cluster at YITP, and CESGA’s Finis Terrae.
Funding AgencyGrant Number
European Research Council (ERC)DyBHo-256667
Science and Technology Facilities Council (STFC)ST/I002006/1
COSMOS supercomputer infrastructureUNSPECIFIED
Centro de Supercomputacion de Galicia (CESGA)ICTS-2013-249
Perimeter Institute for Theoretical PhysicsUNSPECIFIED
Fundação para a Ciência e a Tecnologia (FCT)PTDC/FIS/116625/2010
Fundação para a Ciência e a Tecnologia (FCT)CERN/FP/123593/2011
Government of Canada Industry CanadaUNSPECIFIED
Province of Ontario Ministry of Economic Development InnovationUNSPECIFIED
Issue or Number:4
Classification Code:PACS numbers: 04.25.D-, 04.25.dg, 04.40.Nr
Record Number:CaltechAUTHORS:20140821-090717994
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Official Citation:Zilhão, M., Cardoso, V., Herdeiro, C., Lehner, L., & Sperhake, U. (2014). Collisions of oppositely charged black holes. Physical Review D, 89(4), 044008.
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:48762
Deposited By: Jason Perez
Deposited On:21 Aug 2014 21:30
Last Modified:10 Nov 2021 18:35

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