In adiabatically stratified cluster gas the MTI saturates via large plumes destroyed by shear, producing turbulent kinetic energy that scales as χ ω_T.
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3 Pith papers cite this work. Polarity classification is still indexing.
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3D wind-tunnel simulations in the χ~10^3 regime show clump-cocoon geometry sets SB_X/SB_Hα~3, with Hα fraction fixed by atomic physics and X-ray fraction set by residence time in the X-ray band that scales inversely with pressure.
Three-dimensional three-temperature simulations of colliding supersonic plasma flows from irradiated CH mesh targets produce a persistent shocked turbulent mixing layer that evolves toward an isothermal state with anisotropic Reynolds stress and effective Reynolds number around 200.
citing papers explorer
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Magneto-Thermal Instability in Galaxy Clusters -- III. The Limit of Adiabatic Stratification
In adiabatically stratified cluster gas the MTI saturates via large plumes destroyed by shear, producing turbulent kinetic energy that scales as χ ω_T.
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Clumps in a Cocoon: Geometry and Mixing Set the Universal X-ray to H$\alpha$ Surface Brightness Ratio
3D wind-tunnel simulations in the χ~10^3 regime show clump-cocoon geometry sets SB_X/SB_Hα~3, with Hα fraction fixed by atomic physics and X-ray fraction set by residence time in the X-ray band that scales inversely with pressure.
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Numerical simulations of shock-driven, supersonic turbulence in colliding three-temperature laboratory plasmas
Three-dimensional three-temperature simulations of colliding supersonic plasma flows from irradiated CH mesh targets produce a persistent shocked turbulent mixing layer that evolves toward an isothermal state with anisotropic Reynolds stress and effective Reynolds number around 200.