In AWSoM, switching from a non-conservative to a conservative energy equation raises CME kinetic energy by 232%, with hotter current-sheet pressure prolonging reconnection.
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6 Pith papers cite this work. Polarity classification is still indexing.
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Pith papers citing it
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astro-ph.SR 6years
2026 6representative citing papers
An automated detection method applied to simulated flare ribbon data identifies fine structures whose motions and flux distribution are consistent with plasmoid-mediated reconnection.
A coupled nested-grid MHD framework with AMR to 700 km resolution and Boris correction for strong fields enables end-to-end simulation of CME emergence, eruption, and heliospheric propagation from realistic active-region scales.
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.
SKA's sensitivity, bandwidth and frequency coverage will enable routine radio diagnostics of CME magnetic fields that current precursors can only demonstrate sporadically, improving space-weather models.
citing papers explorer
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The Effects of Energy Conservation in Simulating Solar Eruptions
In AWSoM, switching from a non-conservative to a conservative energy equation raises CME kinetic energy by 232%, with hotter current-sheet pressure prolonging reconnection.
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Automatic detection of Flare Ribbon Fine Structures as Proxies for Plasmoid Dynamics in Flare Reconnection
An automated detection method applied to simulated flare ribbon data identifies fine structures whose motions and flux distribution are consistent with plasmoid-mediated reconnection.
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Modeling of Coronal Mass Ejection Originated from a Sheared Arcade of Realistic Active-Region Scale and Its Propagation in the Heliosphere: Methodology
A coupled nested-grid MHD framework with AMR to 700 km resolution and Boris correction for strong fields enables end-to-end simulation of CME emergence, eruption, and heliospheric propagation from realistic active-region scales.
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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.
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Role of SKA in Advancing Remote Measurements of Magnetic Fields of Solar Coronal Mass Ejections
SKA's sensitivity, bandwidth and frequency coverage will enable routine radio diagnostics of CME magnetic fields that current precursors can only demonstrate sporadically, improving space-weather models.