Nonlinear mixing behavior of the three-dimensional Rayleigh–Taylor instability at a decelerating interface

Drake, R. P.; Leibrandt, David R.; Harding, Eric; Kuranz, Carolyn; Blackburn, Michael; Robey, H. F.; Remington, B. A.; Edwards, M. J.; Miles, A. R.; Perry, T. S.; Wallace, R. J.; Louis, H.; Knauer, J. P.; Arnett, David

doi:10.1063/1.1651492

Cited by 49 publications

(49 citation statements)

References 34 publications

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“…However, there are no 3D simulations of SN explosions, and the velocities remain too small to explain SN 1987A in 3D simulations 63,[73][74][75] and buoyancy-drag models 76,77 of isolated 3D spikes. Other existing studies of 3D RT instabilities, reviewed in Drake et al, 24 are of limited relevance for reasons discussed there.…”

Section: Structure In Supernovae a Importance Of The Workmentioning

confidence: 99%

“…These spikes were much longer that typical buoyancydrag models would predict. 24 It is quite clear that initial conditions determine how far the spikes penetrate. [This has also been seen in hydrodynamic simulations of planar systems in two dimensions.…”

Section: B Recent Researchmentioning

confidence: 99%

“…Our experiments with specific three-dimensional initial conditions showed much larger transport than one would expect from the relevant simulations. 24 This important result led to improving our measurements and performing a sequence of experiments to explore specific variations in initial conditions. These efforts came to fruition in 2006, when we used dual-axis radiography with backlit pinholes and ungated detectors to obtain highresolution the physics data for a Ph.D. thesis, now under analysis.…”

Section: The Overall Project and Its Relevancementioning

confidence: 99%

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Annual Report 2006 for Hydrodynamics and Radiation Hydrodynamics with Astrophysical Applications

Drake¹

2007

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Target for a supernova hydrodynamics experiment. The large acrylic shield has several advantages.Dual orthogonal backlit pinhole radiographs using ungated detectors. From experiments to study Rayleigh-Taylor evolution from a 3D sinusoidal pattern, at 21 ns. Left: an image across the CHBr strip. Right: an image down the CHBr strip. In both images dense spikes and the shockwave can be seen. They are moving to the right. The grid is for spatial calibration and magnification. The bright white feature on the left is a scratch on the film. Radiograph, of radiative shock in Xe gas after image processing to remove x-ray intensity variations.

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Section: Structure In Supernovae a Importance Of The Workmentioning

confidence: 99%

Section: B Recent Researchmentioning

confidence: 99%

Section: The Overall Project and Its Relevancementioning

confidence: 99%

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Annual Report 2006 for Hydrodynamics and Radiation Hydrodynamics with Astrophysical Applications

Drake¹

2007

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“…Other extensive work has also been undertaken and is ongoing in the context of inertial fusion research. In addition, RT growth has been studied when a blast wave first shocks and then decelerates an embedded interface, in experiments motivated by supernova explosion dynamics [28][29][30][31]. In these cases, there is an initial RM response followed by a longer period of RT growth.…”

Section: Rtmentioning

confidence: 99%

Approaches to turbulence in high-energy-density experiments

Drake

Harding²,

Kuranz³

2008

Phys. Scr.

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This paper provides a discussion of the properties of hydrodynamic systems at high energy density, discusses the methods of doing hydrodynamic experiments and discusses studies to date of the three primary instabilities-Richtmyer-Meshkov (RM), Rayleigh-Taylor (RT) and Kelvin-Helmholtz (KH). The first two of these have been systematically observed, but have not yet produced a system with a clear transition to turbulence. The KH instability remains to be systematically observed in its pure form, although some related effects such as spike tip broadening have been seen. However, the KH effects seen in some simulations of RT systems and supersonic jets have not been seen to date in experiments. We note that the time-dependent condition for turbulence of Zhou et al (2003 Phys. Plasmas 10 1883) is roughly equivalent to the Reynolds-number threshold of Dimotakis in that eddies will dissipate by turbulence in about one eddy-turnover time. We suggest that a plausible explanation of the absence of KH in several experimental systems may be that finite velocity gradients have quenched the instability. Finally, we argue that despite the smearing of the shear layer caused by viscous diffusion, KH instabilities have the potential to contribute to the generation of fluctuations at all scales, but only if the local shear layers are initially formed with a sufficiently steep velocity gradient.

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“…This behavior has been explored in a sequence of experiments, marked by steadily increasing precision of the diagnostics and complexity of the structure. [49][50][51] The potential for surprises exists in the high-Reynolds-number regime of these flows, which cannot be fully simulated, especially if fluid turbulence develops as the structures evolve.…”

Section: Relevant Laboratory Experimentsmentioning

confidence: 99%

Stellar explosions, instabilities, and turbulence

Drake¹,

Kuranz²,

Miles³

et al. 2009

Physics of Plasmas

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It has become very clear that the evolution of structure during supernovae is centrally dependent on the pre-existing structure in the star. Modeling of the pre-existing structure has advanced significantly, leading to improved understanding and to a physically based assessment of the structure that will be present when a star explodes. It remains an open question whether low-mode asymmetries in the explosion process can produce the observed effects or whether the explosion mechanism somehow produces jets of material. In any event, the workhorse processes that produce structure in an exploding star are blast-wave driven instabilities. Laboratory experiments have explored these blast-wave-driven instabilities and specifically their dependence on initial conditions. Theoretical work has shown that the relative importance of Richtmyer-Meshkov and RayleighTaylor instabilities varies with the initial conditions and does so in ways that can make sense of a range of astrophysical observations.

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Nonlinear mixing behavior of the three-dimensional Rayleigh–Taylor instability at a decelerating interface

Cited by 49 publications

References 34 publications

Annual Report 2006 for Hydrodynamics and Radiation Hydrodynamics with Astrophysical Applications

Annual Report 2006 for Hydrodynamics and Radiation Hydrodynamics with Astrophysical Applications

Approaches to turbulence in high-energy-density experiments

Stellar explosions, instabilities, and turbulence

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