How to move a black hole without excision: Gauge conditions for the numerical evolution of a moving puncture

By J. V. Meter, John G. Baker, M. Koppitz, Dae-Il Choi. 2006

161 citations recorded by the source corpus.

Recent demonstrations of unexcised black holes traversing across computational grids represent a significant advance in numerical relativity. Stable and accurate simulations of multiple orbits, and their radiated waves, result. This capability is critically undergirded by a careful choice of gauge. Here we present analytic considerations which suggest certain gauge choices, and numerically demonstrate their efficacy in evolving a single moving puncture black hole.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/e7664232e0b06bd0724b3d2d3ace646de56fc596

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Citations in the corpus

Getting a Kick Out of Numerical Relativity (2006, methodology): “The punctures are allowed to move freely through the grid and are evolved according to a variant of the BaumgarteShapiro-Shibata-Nakamura formulation of Einstein’s equations and gauge conditions as described in Baker et al. (2006b); van Meter et al. (2006).”
Beyond second-order convergence in simulations of binary neutron stars in full general-relativity (2013, methodology): “Our gauges are the standard1 + log slicing condition (Bona et al. 1995) and the moving puncture spatial gauge condition (van Meter et al. 2006)with damping parameter set to0.”
Turduckening black holes: An Analytical and computational study (2008, methodology): “Note that we use the operator ∂̂0 (as opposed to ∂t) in these gauge conditions; not only does this simplify the analysis of the principal part of the evolution equations, it also results in stable binary black hole evolutions for moving punctures [16] and the turducken approach [1].”
Black-hole binaries, gravitational waves, and numerical relativity (2010, background): “(23) and (24) can be integrated to yield Bi = Γ̃i − 43ηββi; this substitution allows the removal of the equation for Bi, leaving only a single shift equation (van Meter et al., 2006a): ∂tβ i = 3 4 Γ̃i + βj∂jβ i − ηββi.”