Numerical simulation of orbiting black holes

Bernd Bruegmann; Nina Jansen; Wolfgang Tichy

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Numerical simulation of orbiting black holes

Bernd Bruegmann, Wolfgang Tichy, Nina Jansen

General Relativity and Quantum Cosmology · Submitted 26 Dec 2003

abstract compiled · 2026-09-23 · no language-model review

The authors' main claim We present numerical simulations of binary black hole systems which for the first time last for about one orbital period for close but still separate black holes as indicated by the absence of a common apparent horizon.

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We present numerical simulations of binary black hole systems which for the first time last for about one orbital period for close but still separate black holes as indicated by the absence of a common apparent horizon. An important part of the method is the construction of comoving coordinates, in which both the angular and radial motion is minimized through a dynamically adjusted shift condition. We use fixed mesh refinement for computational efficiency.

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#	sentence	role	the authors' own work	states the main conclusion	strength
s0	We present numerical simulations of binary black hole systems which for the first time last for about one orbital period for close but still separate black holes as indicated by the absence of a common apparent horizon.	contribution 0.84	0.96	0.77	asserted 0.99
s1	An important part of the method is the construction of comoving coordinates, in which both the angular and radial motion is minimized through a dynamically adjusted shift condition.	method 1.00	0.90	0.05	asserted 1.00
s2	We use fixed mesh refinement for computational efficiency.	method 1.00	0.92	0.03	asserted 1.00

What kind of paper the classifier reports this is: simulation study 1.00 · evidence from simulation or computation 1.00.

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The paper

Original abstract

We present numerical simulations of binary black hole systems which for the first time last for about one orbital period for close but still separate black holes as indicated by the absence of a common apparent horizon. An important part of the method is the construction of comoving coordinates, in which both the angular and radial motion is minimized through a dynamically adjusted shift condition. We use fixed mesh refinement for computational efficiency.

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Cited by 26 Pith papers

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How the literature uses it

15 arXiv papers cite this in 16 sentences

Each citing sentence is taken from the citing paper's LaTeX source and typed by Pith's classifier. A label appears at probability 0.8 or more (0.95 for support), a contest at 0.7 or more; the quoted words are the citing authors'. How each label was checked · JSON

Papers citing it · 6 sentences without a confident label

Uses its method or tool 5 papers

We performed a parameter study of the black hole binary problem using 3d numerical simulations obtained with the BAM code [ref] .

Eccentric black hole mergers and zoom-whirl behavior from elliptic inspirals to hyperbolic encounters · Method · 1.00
Evolutions were performed with the BAM code described in [ref] .

Tidal effects in binary neutron star coalescence · Numerical simulations · 1.00
We use two different NR codes: [ref] and [ref] .

CoRe database of binary neutron star merger waveforms and its application in waveform development · Simulation Methods · 1.00

Cites it as background 4 papers

Numerical relativity (NR), on the other hand, solves the two-body problem non-perturbatively from the full Einstein field equations [ref] .

Binary black hole scattering with generic spins · Introduction · 0.90
After the series of breakthroughs that ushered in an era of rapid progress in the field [ref] , several investigations assessing the accuracy of the available equal mass waveforms and applying them to data analysis were conducted [ref] .

Mergers of nonspinning black-hole binaries: Gravitational radiation characteristics · Introduction · 0.91
Despite such numerous potential applications, NR binary BH waveforms beyond GR have been historically difficult to produce, echoing the grand challenges that characterised NR before and in the years immediately following the binary BH breakthrough [ref] .

Towards long and accurate numerical relativity waveforms of binary black holes beyond general relativity · Introduction · 0.89

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