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.
The Astrophysical Journal , eprint =
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MHD-PIC simulations find that the non-thermal particle spectral index alpha steepens as alpha proportional to beta to the power 0.5 in the relativistic regime, due to inertial mass density acting as an energy sink that reduces Alfven velocity.
Cosmic ray transport requires a propagator P(k,s) that encodes memory and non-diffusive behaviors rather than being reduced to a single diffusion coefficient.
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.
A neural network detector applied to 2011 solar radio spectra identified 50 QFP wave train candidates, with 13 associated with global coronal EUV waves.
RAT alignment boosted by B-star radiation plus DG alignment reproduces super-Serkowski spectra in HD 30614 and HD 204827 while standard RAT alone fits Serkowski spectra in HD 37903 and HD 161056.
citing papers explorer
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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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The $\beta$-Dependence of Particle Spectra in Relativistic Turbulent Reconnection
MHD-PIC simulations find that the non-thermal particle spectral index alpha steepens as alpha proportional to beta to the power 0.5 in the relativistic regime, due to inertial mass density acting as an energy sink that reduces Alfven velocity.
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Beyond the Diffusion Coefficient: Propagators and Memory in Cosmic Ray Transport
Cosmic ray transport requires a propagator P(k,s) that encodes memory and non-diffusive behaviors rather than being reduced to a single diffusion coefficient.
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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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Detector for fast wave trains in the solar radio emission
A neural network detector applied to 2011 solar radio spectra identified 50 QFP wave train candidates, with 13 associated with global coronal EUV waves.
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Grain Alignment and Dust Evolution Physics with Polarisation (GRADE-POL). II. On the physical basis of Serkowski and super-Serkowski polarisation spectra
RAT alignment boosted by B-star radiation plus DG alignment reproduces super-Serkowski spectra in HD 30614 and HD 204827 while standard RAT alone fits Serkowski spectra in HD 37903 and HD 161056.