Variable Density Fluid Turbulence

Chassaing, Patrick

doi:10.1007/978-94-017-0075-7

Cited by 154 publications

(130 citation statements)

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“…Although the order of magnitude estimates we carried out in this section have no predictive power, they suggest that Equation (44) provides a valuable framework to analyze pressure fluctuations (Chassaing et al 2002). We plan to push the analysis based on this equation further, with the aim of obtaining more quantitive predictions.…”

Section: Magnitude Of Pressure Fluctuationsmentioning

confidence: 99%

Turbulent Convection in Stellar Interiors. Iii. Mean-Field Analysis and Stratification Effects

Viallet

Meakin

Arnett

et al. 2013

ApJ

126

213

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We present three-dimensional implicit large eddy simulations of the turbulent convection in the envelope of a 5 M red giant star and in the oxygen-burning shell of a 23 M supernova progenitor. The numerical models are analyzed in the framework of one-dimensional Reynolds-Averaged Navier-Stokes equations. The effects of pressure fluctuations are more important in the red giant model, owing to larger stratification of the convective zone. We show how this impacts different terms in the mean-field equations. We clarify the driving sources of kinetic energy, and show that the rate of turbulent dissipation is comparable to the convective luminosity. Although our flows have low Mach numbers and are nearly adiabatic, our analysis is general and can be applied to photospheric convection as well. The robustness of our analysis of turbulent convection is supported by the insensitivity of the mean-field balances to linear mesh resolution. We find robust results for the turbulent convection zone and the stable layers in the oxygen-burning shell model, and robust results everywhere in the red giant model, but the mean fields are not well converged in the narrow boundary regions (which contain steep gradients) in the oxygen-burning shell model. This last result illustrates the importance of unresolved physics at the convective boundary, which governs the mixing there.

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Section: Magnitude Of Pressure Fluctuationsmentioning

confidence: 99%

Turbulent Convection in Stellar Interiors. Iii. Mean-Field Analysis and Stratification Effects

Viallet

Meakin

Arnett

et al. 2013

ApJ

126

213

View full text Add to dashboard Cite

show abstract

“…Variable-density and compressibility effects 10 are important in all of the applications mentioned above. In particular, it is important to understand the effects of shocks of various strengths on turbulence and on turbulent mixing layers, including the effects on coherent structures and on the structures resulting from the evolution of the instabilities through baroclinic effects within the mixing layer.…”

Section: Turbulent Mixingmentioning

confidence: 99%

Predictive Academic Alliances Program (PSAAP) Technical White Paper

Schilling¹,

Steinkamp²,

Baer³

2006

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“…Variable-density and compressibility effects 9 are important in all of the applications mentioned above. In particular, it is important to understand the effects of shocks of various strengths on turbulence and on turbulent mixing layers, including the effects on coherent structures and on the structures resulting from the evolution of the instabilities through baroclinic effects within the mixing layer.…”

Section: Turbulent Mixingmentioning

confidence: 99%