A multi-height extrapolation framework using chromospheric vector data recovers a pre-eruptive flux-rope configuration in an observed solar filament, outperforming photosphere-only models in simulation tests.
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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.
In the 2022 March 31 solar flare, hard X-ray QPPs correlate with UV pulsations in stationary ribbon regions tied to a specific loop system in a large-scale 3D reconnection structure, while slipping kernels experience weaker non-thermal energization.
Data-driven simulation of AR 11158 produces an X-flare triggered by torus instability after MFR formation above a cPIL, with energy release and photospheric changes matching some observed trends.
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 simulation of successive flux-rope eruptions shows reconnection flux accumulating linearly with CME velocity, consistent with HMI/AIA observations of one event.
citing papers explorer
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Chromospheric magnetic field extrapolations reveal the flux-rope configuration of a solar filament
A multi-height extrapolation framework using chromospheric vector data recovers a pre-eruptive flux-rope configuration in an observed solar filament, outperforming photosphere-only models in simulation tests.
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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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Quasi-periodic pulsations and three-dimensional magnetic reconnection during 2022 March 31 flare observed by IRIS & STIX
In the 2022 March 31 solar flare, hard X-ray QPPs correlate with UV pulsations in stationary ribbon regions tied to a specific loop system in a large-scale 3D reconnection structure, while slipping kernels experience weaker non-thermal energization.
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Data-inspired simulation of AR 11158
Data-driven simulation of AR 11158 produces an X-flare triggered by torus instability after MFR formation above a cPIL, with energy release and photospheric changes matching some observed trends.
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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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Evolution of reconnection flux during eruption of magnetic flux ropes
3D MHD simulation of successive flux-rope eruptions shows reconnection flux accumulating linearly with CME velocity, consistent with HMI/AIA observations of one event.