Variations of Flaring Kernel Sizes in Various Parts of the H⍺ Line Profile

We analyze the temporal variations of the sizes and emission intensities of 31 flaring kernels in various parts of the H? line profile. We have found that the areas of all kernels decrease systematically when observed in consecutive wavelengths toward the wings of the H? line, but their areas and emission intensity vary in time. Our results are in agreement with the commonly accepted model of the wine-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?ków Observatory of the University of Wroc?aw, Poland.