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.
The Density Probability Distribution in Compressible Isothermal Turbulence: Solenoidal versus Compressive Forcing
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abstract
The probability density function (PDF) of the gas density in turbulent supersonic flows is investigated with high-resolution numerical simulations. In a systematic study, we compare the density statistics of compressible turbulence driven by the usually adopted solenoidal forcing (divergence-free) and by compressive forcing (curl-free). Our results are in agreement with studies using solenoidal forcing. However, compressive forcing yields a significantly broader density distribution with standard deviation ~3 times larger at the same rms Mach number. The standard deviation-Mach number relation used in analytical models of star formation is reviewed and a modification of the existing expression is proposed, which takes into account the ratio of solenoidal and compressive modes of the turbulence forcing.
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Molecular gas in M83 consists of two log-normal density components, with the high-density component enhanced along spiral arms and more tightly linked to star formation than the low-density component.
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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.
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Sub-kpc scale gas density histograms of the nearby barred spiral galaxy M83: Multi-component molecular gas structure reflecting the galactic environment
Molecular gas in M83 consists of two log-normal density components, with the high-density component enhanced along spiral arms and more tightly linked to star formation than the low-density component.