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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6 Pith papers cite this work. Polarity classification is still indexing.
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UNVERDICTED 6representative citing papers
SuNeRF-CME uses physics-informed NeRFs with ray-tracing for Thomson scattering and constraints on plasma continuity, direction, and speed to enable tomographic 3D reconstruction of CMEs from as few as two viewpoints, validated on synthetic data with low parameter errors.
Analysis of the September 6, 2011 coronal wave with the SOLERwave multi-sector method reveals over 40% speed variation (750-1500 km/s) between northward and northwestward segments, attributed to differences in magnetosonic speed from an MHD solution.
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.
Persistent same-polarity flux emergences drove collisional shearing and cancellations at a PIL, accumulating free energy and forming MFRs that produced multiple large flares including X9.0, with a pre-flare drop in photospheric free-energy area as a possible precursor.
Pre-flare IRIS observations of an X9 flare reveal 7-21 minute oscillations and rising Si IV velocities consistent with slow coronal magnetic destabilization before rapid reconnection.
citing papers explorer
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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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SuNeRF-CME: Physics-Informed Neural Radiance Fields for Tomographic Reconstruction of Coronal Mass Ejections
SuNeRF-CME uses physics-informed NeRFs with ray-tracing for Thomson scattering and constraints on plasma continuity, direction, and speed to enable tomographic 3D reconstruction of CMEs from as few as two viewpoints, validated on synthetic data with low parameter errors.
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Investigation of the Two-Dimensional Velocity Field of the Large-Scale Coronal Wave from September 6, 2011 using the SOLERwave Tool
Analysis of the September 6, 2011 coronal wave with the SOLERwave multi-sector method reveals over 40% speed variation (750-1500 km/s) between northward and northwestward segments, attributed to differences in magnetosonic speed from an MHD solution.
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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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Magnetic Evolution of Highly-Sheared Region in Active Region 13842 Producing Large X9.0 Flare
Persistent same-polarity flux emergences drove collisional shearing and cancellations at a PIL, accumulating free energy and forming MFRs that produced multiple large flares including X9.0, with a pre-flare drop in photospheric free-energy area as a possible precursor.
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Investigating Pre-flare Signatures in Spectroscopic Observations of an X9-class Solar Flare
Pre-flare IRIS observations of an X9 flare reveal 7-21 minute oscillations and rising Si IV velocities consistent with slow coronal magnetic destabilization before rapid reconnection.