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Title: Rayleigh–Taylor and Richtmyer–Meshkov instability induced flow, turbulence, and mixing. II

Abstract

Rayleigh–Taylor (RT) and Richtmyer–Meshkov(RM) instabilities are well-known pathways towards turbulent mixing layers, in many cases characterized by significant mass and species exchange across the mixing layers (Zhou, 2017. Physics Reports, 720–722, 1–136). Mathematically, the pathway to turbulent mixing requires that the initial interface be multimodal, to permit cross-mode coupling leading to turbulence. Practically speaking, it is difficult to experimentally produce a non-multi-mode initial interface. Numerous methods and approaches have been developed to describe the late, multimodal, turbulent stages of RT and RM mixing layers. This paper first presents the initial condition dependence of RT mixing layers, and introduces parameters that are used to evaluate the level of “mixedness” and “mixed mass” within the layers, as well as the dependence on density differences, as well as the characteristic anisotropy of this acceleration-driven flow, emphasizing some of the key differences between the two-dimensional and three-dimensional RT mixing layers.

Authors:
 [1]
  1. Lawrence Livermore National Lab. (LLNL), Livermore, CA (United States)
Publication Date:
Research Org.:
Lawrence Livermore National Lab. (LLNL), Livermore, CA (United States)
Sponsoring Org.:
USDOE National Nuclear Security Administration (NNSA)
OSTI Identifier:
1569184
Report Number(s):
LLNL-JRNL-751112
Journal ID: ISSN 0370-1573; 936444; TRN: US2100266
Grant/Contract Number:  
AC52-07NA27344
Resource Type:
Accepted Manuscript
Journal Name:
Physics Reports
Additional Journal Information:
Journal Volume: 723-725; Journal Issue: C; Journal ID: ISSN 0370-1573
Publisher:
Elsevier
Country of Publication:
United States
Language:
English
Subject:
70 PLASMA PHYSICS AND FUSION TECHNOLOGY; Rayleigh–Taylor instability; Richtmyer–Meshkov instability; Kelvin–Helmholtz instability; Shock waves; Transition; Turbulence; Mixing; Astrophysical fluid dynamics; SuperNovae; Inertial confinement fusion (ICF); High energy density physics (HEDP); Direct numerical simulations (DNS); Large-eddy simulations (LES)

Citation Formats

Zhou, Ye. Rayleigh–Taylor and Richtmyer–Meshkov instability induced flow, turbulence, and mixing. II. United States: N. p., 2017. Web. doi:10.1016/j.physrep.2017.07.008.
Zhou, Ye. Rayleigh–Taylor and Richtmyer–Meshkov instability induced flow, turbulence, and mixing. II. United States. https://doi.org/10.1016/j.physrep.2017.07.008
Zhou, Ye. Wed . "Rayleigh–Taylor and Richtmyer–Meshkov instability induced flow, turbulence, and mixing. II". United States. https://doi.org/10.1016/j.physrep.2017.07.008. https://www.osti.gov/servlets/purl/1569184.
@article{osti_1569184,
title = {Rayleigh–Taylor and Richtmyer–Meshkov instability induced flow, turbulence, and mixing. II},
author = {Zhou, Ye},
abstractNote = {Rayleigh–Taylor (RT) and Richtmyer–Meshkov(RM) instabilities are well-known pathways towards turbulent mixing layers, in many cases characterized by significant mass and species exchange across the mixing layers (Zhou, 2017. Physics Reports, 720–722, 1–136). Mathematically, the pathway to turbulent mixing requires that the initial interface be multimodal, to permit cross-mode coupling leading to turbulence. Practically speaking, it is difficult to experimentally produce a non-multi-mode initial interface. Numerous methods and approaches have been developed to describe the late, multimodal, turbulent stages of RT and RM mixing layers. This paper first presents the initial condition dependence of RT mixing layers, and introduces parameters that are used to evaluate the level of “mixedness” and “mixed mass” within the layers, as well as the dependence on density differences, as well as the characteristic anisotropy of this acceleration-driven flow, emphasizing some of the key differences between the two-dimensional and three-dimensional RT mixing layers.},
doi = {10.1016/j.physrep.2017.07.008},
journal = {Physics Reports},
number = C,
volume = 723-725,
place = {United States},
year = {2017},
month = {9}
}

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Figures / Tables:

Fig. 9.1 Fig. 9.1: (Figure 13 of Ramaprabhu et al., 2005, J. Fluid Mech. with permission). Effect of $k$⟨$h$$k$0⟩: (a) Evolution of bubble amplitude, $h$$b$ for three cases with long wavelengths present in the initial conditions; (b) Evolution of bubble amplitude, $h$$b$ for mode-coupling cases.

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