High-resolution Fe I and Mg I spectral observations reveal that solar flare ribbons are modulated by stable uncombed chromospheric loops and non-flaring fine structures.
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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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Solar flare ribbons structured by uncombed chromospheric loops
High-resolution Fe I and Mg I spectral observations reveal that solar flare ribbons are modulated by stable uncombed chromospheric loops and non-flaring fine structures.
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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.