A model based on Chandrasekhar's 1951 time-invariant quantity quantitatively explains the Mach-number dependence of the density power spectrum slope in isothermal supersonic turbulence and demonstrates that the slope cannot reliably determine the Mach number.
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Kpc-resolution ALMA CO and dust maps of three z~3 dusty galaxies are consistent with gravo-turbulent star-formation models rather than non-turbulent predictions.
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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The slope of the power spectrum of the density field in isothermal supersonic compressible turbulence
A model based on Chandrasekhar's 1951 time-invariant quantity quantitatively explains the Mach-number dependence of the density power spectrum slope in isothermal supersonic turbulence and demonstrates that the slope cannot reliably determine the Mach number.
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Investigating the role of turbulence in the interstellar medium in $z\sim3$ dusty star-forming galaxies using kpc-resolution ALMA dust and gas maps
Kpc-resolution ALMA CO and dust maps of three z~3 dusty galaxies are consistent with gravo-turbulent star-formation models rather than non-turbulent predictions.
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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.