Non-Gaussian Si IV profiles are common (~60%) in the solar transition region and strongly depend on the angle between the magnetic field and line of sight, with k-like shapes more prevalent at large angles.
Title resolution pending
4 Pith papers cite this work. Polarity classification is still indexing.
4
Pith papers citing it
years
2026 4verdicts
UNVERDICTED 4representative 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.
The paper reviews electron transport in tangled magnetic fields, including creation via turbulence, modulation by instabilities, trapping, cross-field diffusion, and energization.
Observational evidence points to the chromosphere as the site of chemical fractionation responsible for the FIP effect in the solar corona.
citing papers explorer
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Anisotropic non-Maxwellian velocity distributions in the solar transition region
Non-Gaussian Si IV profiles are common (~60%) in the solar transition region and strongly depend on the angle between the magnetic field and line of sight, with k-like shapes more prevalent at large angles.
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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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Transport of electrons in tangled magnetic fields
The paper reviews electron transport in tangled magnetic fields, including creation via turbulence, modulation by instabilities, trapping, cross-field diffusion, and energization.
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The connection between solar coronal abundances and the underlying lower atmospheric properties
Observational evidence points to the chromosphere as the site of chemical fractionation responsible for the FIP effect in the solar corona.