A Runge-Kutta-Gegenbauer super-time-stepping method for stable, efficient handling of anisotropic non-ideal MHD diffusion.
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2D RMHD simulations show recollimation distance decreases monotonically with magnetization σ, converging to z_MHD/z_HD ∝ (B₀²/P_ext)^{-1/3} in the high-σ regime, with toroidal fields producing localized emission knots and poloidal fields shifting the zone downstream.
3D MHD simulations of young massive star clusters find proton acceleration to hundreds of TeV near O-star termination shocks, with even faster acceleration to over 100 TeV in under 100 years when a supernova remnant expands inside the core.
citing papers explorer
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A robust super-time-stepping scheme for Ohmic and ambipolar diffusion
A Runge-Kutta-Gegenbauer super-time-stepping method for stable, efficient handling of anisotropic non-ideal MHD diffusion.
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2D magnetohydrodynamic jet simulations: properties of recollimation shocks
2D RMHD simulations show recollimation distance decreases monotonically with magnetization σ, converging to z_MHD/z_HD ∝ (B₀²/P_ext)^{-1/3} in the high-σ regime, with toroidal fields producing localized emission knots and poloidal fields shifting the zone downstream.
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Direct simulations of very high energy cosmic ray acceleration in 3D MHD model of a compact star cluster
3D MHD simulations of young massive star clusters find proton acceleration to hundreds of TeV near O-star termination shocks, with even faster acceleration to over 100 TeV in under 100 years when a supernova remnant expands inside the core.