The 3-dimensional Einstein-Klein-Gordon system in characteristic numerical relativity

A. Da Silva; J. Winicour; L. Lehner; L. Rosales; R. Gomez; W. Barreto

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The 3-dimensional Einstein-Klein-Gordon system in characteristic numerical relativity

W. Barreto, A. Da Silva, R. Gomez, L. Lehner, L. Rosales, J. Winicour

General Relativity and Quantum Cosmology · Submitted 14 Dec 2004

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

The authors' main claim The amplitudes of the scalar and gravitational outgoing radiation modes exhibit the predicted power law scaling with respect to the amplitude of the initial data.

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arXiv IDgr-qc/0412066 (version 1)

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CitationA. Da Silva, J. Winicour, L. Lehner, L. Rosales, R. Gomez, W. Barreto. "The 3-dimensional Einstein-Klein-Gordon system in characteristic numerical relativity." arXiv:gr-qc/0412066 (2004). https://pith.science/paper/S5UVFJ4N

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What the abstract itself states, as probabilities: claims first 0.03 · states limitation 0.08 · human participants 0.01 · controlled comparison 0.04 · randomized assignment 0.01 · states quantitative result 0.39 · compares with prior results 0.68 · mentions code or data availability 0.03.

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We incorporate a massless scalar field into a 3-dimensional code for the characteristic evolution of the gravitational field. The extended 3-dimensional code for the Einstein--Klein--Gordon system is calibrated to be second order convergent. It provides an accurate calculation of the gravitational and scalar radiation at infinity. As an application, we simulate the fully nonlinear evolution of an asymmetric scalar pulse of ingoing radiation propagating toward an interior Schwarzschild black hole and compute the backscattered scalar and gravitational outgoing radiation patterns. The amplitudes of the scalar and gravitational outgoing radiation modes exhibit the predicted power law scaling with respect to the amplitude of the initial data. For the scattering of an axisymmetric scalar field, the final ring down matches the complex frequency calculated perturbatively for the $\ell=2$ quasinormal mode.

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What the classifier reports for each sentence. The number is the probability it gave the label.
#	sentence	role	the authors' own work	states the main conclusion	strength
s0	We incorporate a massless scalar field into a 3-dimensional code for the characteristic evolution of the gravitational field.	contribution 0.82	0.94	0.05	asserted 1.00
s1	The extended 3-dimensional code for the Einstein--Klein--Gordon system is calibrated to be second order convergent.	method 0.76	0.91	0.10	asserted 1.00
s2	It provides an accurate calculation of the gravitational and scalar radiation at infinity.	result 0.40	0.87	0.11	asserted 1.00
s3	As an application, we simulate the fully nonlinear evolution of an asymmetric scalar pulse of ingoing radiation propagating toward an interior Schwarzschild black hole and compute the backscattered scalar and gravitational outgoing radiation patterns.	contribution 0.82	0.97	0.16	asserted 1.00
s4	The amplitudes of the scalar and gravitational outgoing radiation modes exhibit the predicted power law scaling with respect to the amplitude of the initial data.	result 0.99	0.90	0.23	asserted 1.00
s5	For the scattering of an axisymmetric scalar field, the final ring down matches the complex frequency calculated perturbatively for the $\ell=2$ quasinormal mode.	result 0.99	0.87	0.17	asserted 1.00

What kind of paper the classifier reports this is: simulation study 0.58 · evidence from simulation or computation 1.00.

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Original abstract

We incorporate a massless scalar field into a 3-dimensional code for the characteristic evolution of the gravitational field. The extended 3-dimensional code for the Einstein--Klein--Gordon system is calibrated to be second order convergent. It provides an accurate calculation of the gravitational and scalar radiation at infinity. As an application, we simulate the fully nonlinear evolution of an asymmetric scalar pulse of ingoing radiation propagating toward an interior Schwarzschild black hole and compute the backscattered scalar and gravitational outgoing radiation patterns. The amplitudes of the scalar and gravitational outgoing radiation modes exhibit the predicted power law scaling with respect to the amplitude of the initial data. For the scattering of an axisymmetric scalar field, the final ring down matches the complex frequency calculated perturbatively for the $\ell=2$ quasinormal mode.

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References

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4 arXiv papers cite this in 13 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 · 7 sentences without a confident label

Builds on it 1 paper

Treating the Einstein-Klein-Gordon model problem consistently within the LEO framework requires some modifications to [ref] , specifically to the wave equation for the scalar field ($□ϕ=0$) which is given by Eqs. (21)-(27) of [ref] .

A framework for large-scale relativistic simulations in the characteristic approach · A three–dimensional massless scalar field scattered off a Schwarzschild black hole · 0.85

Uses its method or tool 1 paper

Approximating the integrand by its value at the center $C$ of the parallelogram (evaluated using average values between the points $P$ and $S$), we have then [equation] The evolution algorithm for the metric function $J$ follows the procedure outlined in [ref] .

A framework for large-scale relativistic simulations in the characteristic approach · Evolution equations · 0.99

Cites it as support 1 paper

As work on the characteristic formulation to date illustrates [ref] , it is clear that most three-dimensional characteristic simulations, even vacuum simulations [ref] are resolution-limited.

A framework for large-scale relativistic simulations in the characteristic approach · Introduction · 0.96

Cites it as background 1 paper

Early applications of the characteristic evolution were focused on simulating generic three-dimensional (3D) single-black-hole spacetimes [ref] , Einstein-perfect fluid systems [ref] , Einstein-Klein-Gordon systems [ref] , (nonlinear) perturbations of BHs [ref] , event horizons [ref] , fissioning white holes [ref] , extreme mass ratio inspirals [ref] , stellar core collapse [ref] , as well as linearized systems [ref] .

Fully relativistic three-dimensional Cauchy-characteristic matching for physical degrees of freedom · Introduction · 0.96

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