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Accurate black hole evolutions by fourth-order numerical relativity

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arxiv gr-qc/0505055 v2 pith:JGJUANQ6 submitted 2005-05-12 gr-qc

Y. Zlochower , J. G. Baker , M. Campanelli , C. O. Lousto This is my paper · ORCID
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keywords numericalaccuracyblackfourth-orderrelativityapplybinarydemonstrating
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We present techniques for successfully performing numerical relativity simulations of binary black holes with fourth-order accuracy. Our simulations are based on a new coding framework which currently supports higher order finite differencing for the BSSN formulation of Einstein's equations, but which is designed to be readily applicable to a broad class of formulations. We apply our techniques to a standard set of numerical relativity test problems, demonstrating the fourth-order accuracy of the solutions. Finally we apply our approach to binary black hole head-on collisions, calculating the waveforms of gravitational radiation generated and demonstrating significant improvements in waveform accuracy over second-order methods with typically achievable numerical resolution.

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Cited by 2 Pith papers

Reviewed papers in the Pith corpus that reference this work. Sorted by Pith novelty score. Full citation record

  1. Parameter Estimation with Targeted Eccentric Numerical-Relativity Simulations for GW200208_22 and GW190620

    gr-qc 2025-07 unverdicted novelty 5.0 of 10

    Bayesian parameter estimation with targeted eccentric numerical-relativity waveforms yields eccentricity estimates of e20 ≈ 0.2 for GW200208_22 and e10 ≈ 0.19 for GW190620, reinforcing the eccentric hypothesis.

  2. AthenaK simulations of the binary black hole merger GW150914

    gr-qc 2025-06 conditional novelty 5.0 of 10

    A new open-source GPU code, AthenaK, reproduces the GW150914 merger: remnant mass within 0.01%, spin within 0.02%, and waveform phase within about 0.35 radians of established simulations.

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