Variations of flaring kernel sizes in various parts of the H-alpha line profile

TL;DR

This study investigates how the sizes and intensities of flaring kernels vary across different parts of the H-alpha line profile, revealing systematic size decreases toward the line wings and temporal variations consistent with magnetic loop models.

Contribution

It provides detailed observational evidence of flaring kernel size and intensity variations across the H-alpha line, supporting the glass-shaped magnetic loop model.

Findings

Kernel areas decrease toward the H-alpha line wings.

Kernel sizes and intensities vary over time.

Results support the magnetic loop channeling model.

Abstract

We analyze the temporal variations of the sizes and emission intensities of thirtyone flaring kernels in various parts of the H{\alpha} line profile. We have found that the areas of all kernels decrease systematically when observed in consecutive wavelengths toward the wings of the H{\alpha} line, but their areas and emission intensity vary in time. Our results are in agreement with the commonly accepted model of the glass-shaped lower parts of the magnetic flaring loops channelling high energy variable particle beams toward the chromospheric plasma. High time resolution spectral-imaging data used in our work were collected using the Large Coronagraph and Horizontal Telescope equipped with the Multi-channel Subtractive Double Pass Spectrograph and the Solar Eclipse Coronal Imaging System (MSDP-SECIS) at the Bia{\l}k\'ow Observatory of the University of Wroc{\l}aw, Poland.