The 8.2 μm mid-IR channel in solar flare footpoints peaks 0.3-0.45 s before the 5.2 μm channel due to wavelength-dependent opacity changes from flare-induced ionization.
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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.
citing papers explorer
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First time delay observation between two mid-infrared channels in solar flare footpoints
The 8.2 μm mid-IR channel in solar flare footpoints peaks 0.3-0.45 s before the 5.2 μm channel due to wavelength-dependent opacity changes from flare-induced ionization.
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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.