Type II radio burst sources align with quasi-perpendicular shock regions of enhanced Mach number in the simulation, with fundamental-harmonic offsets matching the projected shock-surface magnetic field direction.
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Background magnetic field orientation affects eruption success and reconnection in MHD simulations of pre-existing flux ropes, with antiparallel fields enabling faster but shorter flare reconnection.
citing papers explorer
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Radio Spectral Imaging and MHD Modeling of a CME-Driven Shock: Connecting Solar Type II Radio Bursts with Shock-Surface Magnetic Geometry
Type II radio burst sources align with quasi-perpendicular shock regions of enhanced Mach number in the simulation, with fundamental-harmonic offsets matching the projected shock-surface magnetic field direction.
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Effects of the Background Magnetic Field on Flux Rope Eruptions
Background magnetic field orientation affects eruption success and reconnection in MHD simulations of pre-existing flux ropes, with antiparallel fields enabling faster but shorter flare reconnection.