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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Energy-conserving numerics in CME simulations yield >2x higher kinetic energy by extending flare reconnection duration compared to non-conservative schemes.
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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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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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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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.