Numerical simulations of Rayleigh–Taylor and Richtmyer–Meshkov instability using MAH-3 code

Anuchina, N. N.; Volkov, Vasily; Gordeychuk, V.A.; Es'kov, N. S.; Ilyutina, O. S.; Kozyrev, O. M.

doi:10.1016/j.cam.2003.06.008

Cited by 35 publications

(21 citation statements)

References 11 publications

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“…Smaller wavelengths grow faster than longer wavelengths, so longer wavelength perturbations are less likely to become nonlinear. In these models, as well as the single instability investigated in Anuchina et al (2004), the RT fingers did not interact with one another, ensuring that the relative drag on the fingers was the only significant difference between 2D and 3D. This accounts for the around 30% faster growth rates discovered in these simulations.…”

Section: Discussionmentioning

confidence: 55%

“…This was found in a laboratory context in the simulations of Miles et al (2005). For simulations in which interactions between the RT fingers do not occur, either because only one finger is modeled (Anuchina et al 2004) or the RT fingers grow for a short enough time that they never interact (Kane et al 2000), the greater effective drag experienced in 2D versus 3D will continue to dominate the simulation, ensuring that the width of the mixed region will be larger in 3D than in 2D. For simulations in which the RT instability has enough time to grow that the fingers begin to interact with one another, the width of the mixed region will be the same in 2D and 3D simulations.…”

Section: Discussionmentioning

confidence: 82%

“…Studies of the RT instability outside the context of SN explosions have also found that a single RT instability grows about 30% faster in 3D than in 2D (Anuchina et al 2004). Previous simulations of the RT instability in a laboratory context (Miles et al 2005) have found that the width of the mixed region is very similar between 3D and 2D, provided that the individual RT fingers interact.…”

Section: Discussionmentioning

confidence: 91%

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Three-Dimensional Simulations of Rayleigh-Taylor Mixing in Core-Collapse Supernovae

Joggerst

Almgren

Woosley

2010

ApJ

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We present multidimensional simulations of the post-explosion hydrodynamics in three different 15 M supernova models with zero, 10 −4 Z , and Z metallicities. We follow the growth of the Rayleigh-Taylor (RT) instability that mixes together the stellar layers in the wake of the explosion. Models are initialized with spherically symmetric explosions and perturbations are seeded by the grid. Calculations are performed in two-dimensional (2D) axisymmetric and three-dimensional (3D) Cartesian coordinates using the new Eulerian hydrodynamics code, CASTRO. We find as in previous work that RT perturbations initially grow faster in 3D than in 2D. As the RT fingers interact with one another, mixing proceeds to a greater degree in 3D than in 2D, reducing the local Atwood number and slowing the growth rate of the instability in 3D relative to 2D. By the time mixing has stopped, the width of the mixed region is similar in the 2D and 3D simulations provided the RT fingers show significant interaction. Our results imply that 2D simulations of light curves and nucleosynthesis in supernovae that die as red giants may capture the features of an initially spherically symmetric explosion in far less computational time than required by a full 3D simulation. However, capturing large departures from spherical symmetry requires a significantly perturbed explosion. Large-scale asymmetries cannot develop through an inverse cascade of merging RT structures; they must arise from asymmetries in the initial explosion.

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Section: Discussionmentioning

confidence: 55%

Section: Discussionmentioning

confidence: 82%

Section: Discussionmentioning

confidence: 91%

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Three-Dimensional Simulations of Rayleigh-Taylor Mixing in Core-Collapse Supernovae

Joggerst

Almgren

Woosley

2010

ApJ

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“…The behavior of RM instability has been isolated and studied by many authors (e.g., [63,[71][72][73]). The numerical study of RM instability by Anuchina et al [74] showed that the growth rate of perturbations in a 3D case was higher than that in a 2D case at the identical initial amplitudes of perturbation and wavelengths. Li and Zhang [73] used both theoretical analysis and high-resolution numerical simulation to compare 2-D and 3-D growth rates of the RM instability.…”

Section: Three-dimensional Effectsmentioning

confidence: 98%

Hydrodynamic Instabilities in Gaseous Detonations: Comparison of Euler, Navier–Stokes, and Large-Eddy Simulation

Mahmoudi

Karimi

Deiterding

et al. 2014

Journal of Propulsion and Power

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A large-eddy simulation is conducted to investigate the transient structure of an unstable detonation wave in two dimensions and the evolution of intrinsic hydrodynamic instabilities. The dependency of the detonation structure on the grid resolution is investigated, and the structures obtained by large-eddy simulation are compared with the predictions from solving the Euler and Navier-Stokes equations directly. The results indicate that to predict irregular detonation structures in agreement with experimental observations the vorticity generation and dissipation in small scale structures should be taken into account. Thus, large-eddy simulation with high grid resolution is required. In a low grid resolution scenario, in which numerical diffusion dominates, the structures obtained by solving the Euler or Navier-Stokes equations and large-eddy simulation are qualitatively similar. When high grid resolution is employed, the detonation structures obtained by solving the Euler or Navier-Stokes equations directly are roughly similar yet equally in disagreement with the experimental results. For high grid resolution, only the large-eddy simulation predicts detonation substructures correctly, a fact that is attributed to the increased dissipation provided by the subgrid scale model. Specific to the investigated configuration, major differences are observed in the occurrence of unreacted gas pockets in the high-resolution Euler and Navier-Stokes computations, which appear to be fully combusted when large-eddy simulation is employed.

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“…They observe that the effective Atwood number changes owing to the mixing and defined an effective, time-varying Atwood number that collapses previous numerical and experimental data on the mixing layer growth rate. In reference [86], both single-and multi-mode RTI 120 3 simulations are reported with the MAH-3 code. The development of the kinetic energy spectrum is discussed in connection to the onset of self-similarity in the layer growth.…”

Section: (I) Direct Numerical Simulations Of Rayleigh-taylor Instabilmentioning

confidence: 99%

Numerical simulations of two-fluid turbulent mixing at large density ratios and applications to the Rayleigh–Taylor instability

Livescu

2013

Phil. Trans. R. Soc. A.

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A tentative review is presented of various approaches for numerical simulations of two-fluid gaseous mixtures at high density ratios, as they have been applied to the Rayleigh–Taylor instability (RTI). Systems exhibiting such RTI behaviour extend from atomistic sizes to scales where the continuum approximation becomes valid. Each level of description can fit into a hierarchy of theoretical models and the governing equations appropriate for each model, with their assumptions, are presented. In particular, because the compressible to incompressible limit of the Navier–Stokes equations is not unique and understanding compressibility effects in the RTI critically depends on having the appropriate basis for comparison, two relevant incompressible limits are presented. One of these limits has not been considered before. Recent results from RTI simulations, spanning the levels of description presented, are reviewed in connection to the material mixing problem. Owing to the computational limitations, most in-depth RTI results have been obtained for the incompressible case. Two such results, concerning the asymmetry of the mixing and small-scale anisotropy anomaly, as well as the possibility of a mixing transition in the RTI, are surveyed. New lines for further investigation are suggested and it is hoped that bringing together such diverse levels of description may provide new ideas and increased motivation for studying such flows.

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Numerical simulations of Rayleigh–Taylor and Richtmyer–Meshkov instability using MAH-3 code

Cited by 35 publications

References 11 publications

Three-Dimensional Simulations of Rayleigh-Taylor Mixing in Core-Collapse Supernovae

Three-Dimensional Simulations of Rayleigh-Taylor Mixing in Core-Collapse Supernovae

Hydrodynamic Instabilities in Gaseous Detonations: Comparison of Euler, Navier–Stokes, and Large-Eddy Simulation

Numerical simulations of two-fluid turbulent mixing at large density ratios and applications to the Rayleigh–Taylor instability

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