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High accuracy simulations of black hole binaries: Spins anti-aligned with the orbital angular momentum

Chu, Tony and Pfeiffer, Harald P. and Scheel, Mark A. (2009) High accuracy simulations of black hole binaries: Spins anti-aligned with the orbital angular momentum. Physical Review D, 80 (12). Art. No. 124051. ISSN 2470-0010.

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High-accuracy binary black hole simulations are presented for black holes with spins anti-aligned with the orbital angular momentum. The particular case studied represents an equal-mass binary with spins of equal magnitude S/m^2=0.437 57±0.000 01. The system has initial orbital eccentricity ∼4×10^(-5), and is evolved through 10.6 orbits plus merger and ringdown. The remnant mass and spin are M_f=(0.961 109±0.000 003)M and S_f/M_f^2=0.547 81±0.000 01, respectively, where M is the mass during early inspiral. The gravitational waveforms have accumulated numerical phase errors of ≲0.1 radians without any time or phase shifts, and ≲0.01 radians when the waveforms are aligned with suitable time and phase shifts. The waveform is extrapolated to infinity using a procedure accurate to ≲0.01 radians in phase, and the extrapolated waveform differs by up to 0.13 radians in phase and about 1% in amplitude from the waveform extracted at finite radius r=350M. The simulations employ different choices for the constraint damping parameters in the wave zone; this greatly reduces the effects of junk radiation, allowing the extraction of a clean gravitational wave signal even very early in the simulation.

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Pfeiffer, Harald P.0000-0001-9288-519X
Additional Information:© 2009 The American Physical Society. Received 8 September 2009; published 31 December 2009. We would like to thank Lee Lindblom, Béla Szilágyi, and Kip Thorne for helpful discussions and comments.We thank Mike Kesden for computing the final mass and spin predictions from the various analytical models. We are especially grateful to Fan Zhang for computing the extrapolation of the waveforms to infinite radius using methods and a variant of code developed by Mike Boyle and Abdul Mroue. We acknowledge the use of the Spectral Einstein Code (SpEC). This work was supported in part by the Sherman Fairchild Foundation, the Brinson Foundation, by NSF grants PHY-0601459, PHY- 0652995, and DMS-0553302 and by NASA grant NNX09AF97G. H. P. acknowledges support from the Canadian Institute for Advanced Research. Some calculations were done on the Tungsten cluster at NCSA.
Funding AgencyGrant Number
Sherman Fairchild FoundationUNSPECIFIED
Brinson FoundationUNSPECIFIED
NSFPHY- 0652995
Canadian Institute for Advanced ResearchUNSPECIFIED
Issue or Number:12
Classification Code:PACS: 04.25.D-, 04.25.dg, 04.30.-w, 04.30.Db.
Record Number:CaltechAUTHORS:20100120-074713497
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Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:17226
Deposited By: Ruth Sustaita
Deposited On:26 Jan 2010 16:09
Last Modified:09 Mar 2020 13:19

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