High Accuracy Gravitational Waveforms from Black Hole Binary Inspirals Using OpenCL

McKennon, Justin; Forrester, Gary; Khanna, Gaurav

doi:10.48550/arxiv.1206.0270

Cited by 4 publications

(6 citation statements)

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“…Our numerical evolution scheme is implemented using OpenCL/CUDA-based GPGPUcomputing which allows for very long duration and highaccuracy computations within a reasonable time-frame. Numerical errors in the phase and amplitude are typically on the scale of a small fraction of a percent [64,70].…”

Section: A Numerically Solving the Teukolsky Equationmentioning

confidence: 99%

Surrogate model for gravitational wave signals from non-spinning, comparable- to large-mass-ratio black hole binaries built on black hole perturbation theory waveforms calibrated to numerical relativity

Islam,

Field,

Hughes

et al. 2022

Preprint

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We present a reduced-order surrogate model of gravitational waveforms from non-spinning binary black hole systems with comparable to large mass-ratio configurations. This surrogate model, BHPTNRSur1dq1e4, is trained on waveform data generated by point-particle black hole perturbation theory (ppBHPT) with mass ratios varying from 2.5 to 10,000. BHPTNRSur1dq1e4 extends an earlier waveform model, EMRISur1dq1e4, by using an updated transition-to-plunge model, covering longer durations up to 30,500 m1 (where m1 is the mass of the primary black hole), includes several more spherical harmonic modes up to = 10, and calibrates subdominant modes to numerical relativity (NR) data. In the comparable mass-ratio regime, including mass ratios as low as 2.5, the gravitational waveforms generated through ppBHPT agree surprisingly well with those from NR after this simple calibration step. We also compare our model to recent SXS and RIT NR simulations at mass ratios ranging from 15 to 32, and find the dominant quadrupolar modes agree to better than ≈ 10 −3 . We expect our model to be useful to study intermediate-mass-ratio binary systems in current and future gravitational-wave detectors.

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Section: A Numerically Solving the Teukolsky Equationmentioning

confidence: 99%

Surrogate model for gravitational wave signals from non-spinning, comparable- to large-mass-ratio black hole binaries built on black hole perturbation theory waveforms calibrated to numerical relativity

Islam,

Field,

Hughes

et al. 2022

Preprint

Self Cite

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show abstract

“…In the time domain, we use an approach similar to that of Refs. [7,[47][48][49]. First, the Teukolsky equation is rewritten using compactified hyperboloidal coordinates that allow for GW extraction directly at null infinity, while also solving the issue of unphysical reflections from the artificial boundary of the finite computational grid.…”

Section: B Time and Frequency Domain Integratorsmentioning

confidence: 99%

“…Additional details may be found in Refs. [7,[47][48][49], although those refer to an obsolete second-order, Lax-Wendroff numerical scheme. Details on the high-order WENO implementation may be found in Ref.…”

Section: B Time and Frequency Domain Integratorsmentioning

confidence: 99%

Divergences in gravitational-wave emission and absorption from extreme mass ratio binaries

et al. 2021

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A powerful technique to calculate gravitational radiation from binary systems involves a perturbative expansion: if the masses of the two bodies are very different, the "small" body is treated as a point particle of mass m p moving in the gravitational field generated by the large mass M, and one keeps only linear terms in the small mass ratio m p =M. This technique usually yields finite answers, which are often in good agreement with fully nonlinear numerical relativity results, even when extrapolated to nearly comparable mass ratios. Here we study two situations in which the point-particle approximation yields a divergent result: the instantaneous flux emitted by a small body as it orbits the light ring of a black hole, and the total energy absorbed by the horizon when a small body plunges into a black hole. By integrating the Teukolsky (or Zerilli/Regge-Wheeler) equations in the frequency and time domains we show that both of these quantities diverge. We find that these divergences are an artifact of the point-particle idealization, and are able to interpret and regularize this behavior by introducing a finite size for the point particle. These divergences do not play a role in black-hole imaging, e.g., by the Event Horizon Telescope.

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“…In the time domain, we use an approach similar to that of Refs. [7,[46][47][48]. First, the Teukolsky equation is rewritten using compactified hyperboloidal coordinates that allow for GW extraction directly at null infinity, while also solving the issue of unphysical reflections from the artificial boundary of the finite computational grid.…”

Section: B Time and Frequency Domain Integratorsmentioning

confidence: 99%

“…Additional details may be found in Refs. [7,[46][47][48], although those refer to an obsolete second-order, Lax-Wendroff numerical scheme. Details on the high-order WENO implementation may be found in Ref.…”

Section: B Time and Frequency Domain Integratorsmentioning

confidence: 99%

Divergences in gravitational-wave emission and absorption from extreme mass ratio binaries

Barausse,

Berti,

Cardoso

et al. 2021

Preprint

Self Cite

View full text Add to dashboard Cite

A powerful technique to calculate gravitational radiation from binary systems involves a perturbative expansion: if the masses of the two bodies are very different, the "small" body is treated as a point particle of mass mp moving in the gravitational field generated by the large mass M , and one keeps only linear terms in the small mass ratio mp/M . This technique usually yields finite answers, which are often in good agreement with fully nonlinear numerical relativity results, even when extrapolated to nearly comparable mass ratios. Here we study two situations in which the point-particle approximation yields a divergent result: the instantaneous flux emitted by a small body as it orbits the light ring of a black hole, and the total energy absorbed by the horizon when a small body plunges into a black hole. By integrating the Teukolsky (or Zerilli/Regge-Wheeler) equations in the frequency and time domains we show that both of these quantities diverge. We find that these divergences are an artifact of the point-particle idealization, and are able to interpret and regularize this behavior by introducing a finite size for the point particle. These divergences do not play a role in black-hole imaging, e.g. by the Event Horizon Telescope.

show abstract

High Accuracy Gravitational Waveforms from Black Hole Binary Inspirals Using OpenCL

Cited by 4 publications

References 0 publications

Surrogate model for gravitational wave signals from non-spinning, comparable- to large-mass-ratio black hole binaries built on black hole perturbation theory waveforms calibrated to numerical relativity

Surrogate model for gravitational wave signals from non-spinning, comparable- to large-mass-ratio black hole binaries built on black hole perturbation theory waveforms calibrated to numerical relativity

Divergences in gravitational-wave emission and absorption from extreme mass ratio binaries

Divergences in gravitational-wave emission and absorption from extreme mass ratio binaries

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