A comparative study of the turbulent Rayleigh–Taylor instability using high-resolution three-dimensional numerical simulations: The Alpha-Group collaboration

Dimonte, Guy; Youngs, D. L.; Dimits, A. M.; Weber, S. V.; Marinak, M. M.; Wunsch, Scott; Garasi, Christopher J.; Robinson, Allen C.; Andrews, Malcolm J.; Ramaprabhu, Praveen; Calder, A. C.; Fryxell, B.; Biello, Joseph A.; Dursi, L. J.; MacNeice, P. J.; Olson, K.; Ricker, P. M.; Rosner, R.; Timmes, F. X.; Tufo, Henry M.; Young, Yuan-Nan; Zingale, M.

doi:10.1063/1.1688328

Cited by 404 publications

(432 citation statements)

References 67 publications

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“…Similar results were found in numerical studies [26,5]. The RT spike front was found to exhibit similar behavior, h s = α s Agt 2 , where…”

Section: Introductionsupporting

confidence: 73%

Concept Development for Astrophysically Relevant Turbulence on NIF

Drake¹

2012

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(a) Abstract: We carried out the research proposed in the proposal and developed a specific concept for the generation of fully developed Rayleigh-Taylor turbulence on NIF. Under this contract we carried out the design study that we proposed. We demonstrated that NIF is capable of producing self-similar turbulence resulting from the Rayleigh-Taylor instability. Our detailed study shows that NIF can in fact produce a more-developed turbulent state than we estimated in the proposal. Thus, NIF can go far beyond any previous experiment in the generation of a hydrodynamic state that can be described as fully developed turbulence.To accomplish our study, we first assessed what sort of experimental system NIF was capable of driving, for modest values of the laser parameters. We developed a desgin for a specific target that could produce Rayliegh-Taylor turbulentce. We then performed hydrodynamic simulations of of this system. We analyzed the results of these simulations to determine the likely evolution of the turbulence in a NIF experiment.The results of our work are discussed in the following, which is a draft paper for publication. We are now undertaking multidimensional simulations, which will also be included in the paper before it is submitted. 1A preliminary design of a two-dimensional Rayleigh-Taylor experiment on NIF AbstractAn preliminary design of an experiment meant to investigate the evolution of multimode Rayleigh-Taylor instability (RT) is presented. This experiment is intended to provide a direct measurement of the two-dimensional bubble front evolution in the hydrodynamic regime. RT growth for the proposed design has been analyzed using one-dimensional direct numerical simulations in HYADES, and a self-similar behavior model. The proposed design assures a significant bubble merging process (∼ 3-4 bubble merger generations), bringing the bubble front to the self-similar stage. The design takes advantage of the National Ignition Facility (NIF) capabilities to provide a large enough laser spot area (∼0.5-1 cm 2 ), along with a low enough drive, so preheat effects remain reasonably small.

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“…Similar results were found in numerical studies [26,5]. The RT spike front was found to exhibit similar behavior, h s = α s Agt 2 , where…”

Section: Introductionsupporting

confidence: 73%

Concept Development for Astrophysically Relevant Turbulence on NIF

Drake¹

2012

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“…Further analysis on the estimation of θ, analogous to Dimonte et al (2004) and Ristorcelli and Clark (2004) methods applied to estimating the growth rate coefficient for Rayleigh-Taylor mixing, is presented below. If we assume that the growth of the Richtmyer-Meshkov mixing layer is modelled by power-law growth with a virtual time offset…”

Section: Growth Of the Instabilitymentioning

confidence: 99%

Computing multi-mode shock-induced compressible turbulent mixing at late times

et al. 2015

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Both experiments and numerical simulations pertinent to the study of self-similarity in shock-induced turbulent mixing often do not cover sufficiently long enough times for the mixing layer to become developed in a fully turbulent manner. When the Mach number of the flow is sufficiently low, numerical simulations based on the compressible flow equations tend to become less accurate due to inherent numerical cancellation errors. This paper concerns a numerical study of the late time behaviour of single-shocked Richtmyer-Meshkov Instability (RMI) and associated compressible turbulent mixing using a new technique that addresses the above limitation. The present approach exploits the fact that RMI is a compressible flow during the early stages of the simulation and incompressible at late times. Therefore, depending on the compressibility of the flow field the most suitable model, compressible or incompressible, can be employed. This motivates the development of a hybrid compressible-incompressible solver that removes the low-Mach number limitations of the compressible solvers, thus allowing numerical simulations of late time mixing. Simulations have been performed for a multi-mode perturbation at the interface between two fluids of densities corresponding to an Atwood number of 0.5, and results are presented for the development of the instability, mixing parameters and turbulent kinetic energy spectra. The results are discussed in comparison with previous compressible simulations, theory and experiments.

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“…ENZO was used here in version 1.0.1, and FLASH was used in version 2.5. FLASH in particular has been extensively tested against laboratory experiments (Calder et al 2002) and other codes (Dimonte et al 2004;Heitmann et al 2005). For the FLASH run of this work, a PPM diffusion parameter of K = 0.1 (Colella & Woodward 1984) was used, whereas for the ENZO run the PPM diffusion parameter was set to K = 0.0.…”

Section: Experimental Setup and Numerical Codesmentioning

confidence: 99%

Algorithmic comparisons of decaying, isothermal, supersonic turbulence

Kitsionas¹,

Federrath

Klessen

et al. 2009

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120

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Context. Simulations of astrophysical turbulence have reached such a level of sophistication that quantitative results are now starting to emerge. However, contradicting results have been reported in the literature with respect to the performance of the numerical techniques employed for its study and their relevance to the physical systems modelled. Aims. We aim at characterising the performance of a variety of hydrodynamics codes including different particle-based and grid-based techniques on the modelling of decaying supersonic turbulence. This is the first such large-scale comparison ever conducted. Methods. We modelled driven, compressible, supersonic, isothermal turbulence with an rms Mach number of M rms ∼ 4, and then let it decay in the absence of gravity, using runs performed with four different grid codes (ENZO, FLASH, TVD, ZEUS) and three different SPH codes (GADGET, PHANTOM, VINE). We additionally analysed two calculations denoted as PHANTOM A and PHANTOM B using two different implementations of artificial viscosity in PHANTOM. We analysed the results of our numerical experiments using volumeaveraged quantities like the rms Mach number, volume-and density-weighted velocity Fourier spectrum functions, and probability distribution functions of density, velocity, and velocity derivatives. Results. Our analysis indicates that grid codes tend to be less dissipative than SPH codes, though details of the techniques used can make large differences in both cases. For example, the Morris & Monaghan viscosity implementation for SPH results in less dissipation (PHANTOM B and VINE versus GADGET and PHANTOM A). For grid codes, using a smaller diffusion parameter leads to less dissipation, but results in a larger bottleneck effect (our ENZO versus FLASH runs). As a general result, we find that by using a similar number of resolution elements N for each spatial direction means that all codes (both grid-based and particle-based) show encouraging similarity of all statistical quantities for isotropic supersonic turbulence on spatial scales k N/32 (all scales resolved by more than 32 grid cells), while scales smaller than that are significantly affected by the specific implementation of the algorithm for solving the equations of hydrodynamics. At comparable numerical resolution (N particles ≈ N cells ), the SPH runs were on average about ten times more computationally intensive than the grid runs, although with variations of up to a factor of ten between the different SPH runs and between the different grid runs. Conclusions. At the resolutions employed here, the ability to model supersonic to transonic flows is comparable across the various codes used in this study.

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A comparative study of the turbulent Rayleigh–Taylor instability using high-resolution three-dimensional numerical simulations: The Alpha-Group collaboration

Cited by 404 publications

References 67 publications

Concept Development for Astrophysically Relevant Turbulence on NIF

Concept Development for Astrophysically Relevant Turbulence on NIF

Computing multi-mode shock-induced compressible turbulent mixing at late times

Algorithmic comparisons of decaying, isothermal, supersonic turbulence

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