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.
S., Hornig, G., & Démoulin, P
7 Pith papers cite this work, alongside 472 external citations. Polarity classification is still indexing.
7
Pith papers citing it
472
external citations · OpenAlex
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astro-ph.SR 7years
2026 7representative citing papers
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.
Non-force-free initial magnetic fields in solar flare simulations release about twice the magnetic energy and yield EUV emission closer to observations than conventional NLFF extrapolations.
Solar wind composition depends strongly on source distance from the open-closed boundary, with enhanced variability and slow-wind signatures concentrated within ~25 Mm of the boundary.
In NLFFF extrapolations the resistivity-induced field line slippage rate is governed by cross-field gradients of field-aligned twist and serves as a physics-weighted complement to the squashing factor Q for locating reconnection in solar active regions.
Data-constrained 3D modeling of the 2011 August 4 flare reveals strong polarity asymmetry in electron precipitation driven by magnetic mirror ratios, with turbulent scattering and Coulomb collisions modulating the energy-dependent flux.
FastQSL 2 adds dual-spherical-coordinate field-line tracing that eliminates polar singularities and supplies Q_local, footpoint maps, and derived solar-wind and slip-squashing products.
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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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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Energetics and Emission in a Simulated Solar Flare Initialised by a Non-Force Free Magnetic Field
Non-force-free initial magnetic fields in solar flare simulations release about twice the magnetic energy and yield EUV emission closer to observations than conventional NLFF extrapolations.
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Solar Wind Dependence on Source Distance from the Open-Closed Boundary
Solar wind composition depends strongly on source distance from the open-closed boundary, with enhanced variability and slow-wind signatures concentrated within ~25 Mm of the boundary.
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Field line slippage rate signatures in nonlinear force-free field extrapolations
In NLFFF extrapolations the resistivity-induced field line slippage rate is governed by cross-field gradients of field-aligned twist and serves as a physics-weighted complement to the squashing factor Q for locating reconnection in solar active regions.
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Data-Constrained Modeling of Electron Transport and Asymmetric Precipitation in the 2011 August 4 Solar Flare
Data-constrained 3D modeling of the 2011 August 4 flare reveals strong polarity asymmetry in electron precipitation driven by magnetic mirror ratios, with turbulent scattering and Coulomb collisions modulating the energy-dependent flux.
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FastQSL 2: A Comprehensive Toolkit for Magnetic Connectivity Analysis
FastQSL 2 adds dual-spherical-coordinate field-line tracing that eliminates polar singularities and supplies Q_local, footpoint maps, and derived solar-wind and slip-squashing products.