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.
and Zhao, Lulu and Gombosi, Tamas I
5 Pith papers cite this work. Polarity classification is still indexing.
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2026 5verdicts
UNVERDICTED 5representative citing papers
Energy-conserving numerics in CME simulations yield >2x higher kinetic energy by extending flare reconnection duration compared to non-conservative schemes.
MHD simulation of a CME reveals that spacecraft connect to different regions of an inhomogeneous shock, reproducing the observed SEP flux differences among Earth, STA, and SolO.
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.
3D MHD modeling of candle-flame solar flares reveals Y-points do not coincide with apparent cusp tips and observed downflow speeds underestimate reconnection Alfvén speeds by 2-10x.
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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The Effects of Energy Conservation in Simulating Solar Eruptions
Energy-conserving numerics in CME simulations yield >2x higher kinetic energy by extending flare reconnection duration compared to non-conservative schemes.
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Counterintuitive Magnetic Connectivity and Energetic Particle Flux Differences among Nearby Spacecraft During the 2023 February 24 Solar Energetic Particle Event
MHD simulation of a CME reveals that spacecraft connect to different regions of an inhomogeneous shock, reproducing the observed SEP flux differences among Earth, STA, and SolO.
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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.
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On the Nature of Candle-Flame-Shaped Solar Flares and Sub-Alfv\'enic Supra-Arcade Plasma Downflows
3D MHD modeling of candle-flame solar flares reveals Y-points do not coincide with apparent cusp tips and observed downflow speeds underestimate reconnection Alfvén speeds by 2-10x.