Sizes of flaring kernels in various parts of the H-alpha line profile

TL;DR

This study investigates the sizes and intensities of solar flare kernels in different parts of the H-alpha line profile, revealing systematic variations linked to magnetic loop structures and particle beam interactions.

Contribution

It provides new high-resolution spectrophotometric measurements of flaring kernels across the H-alpha line, highlighting their temporal and wavelength-dependent variations.

Findings

Flaring kernel areas vary over time and wavelength.

Kernel intensities decrease toward the wings of the H-alpha line.

Results support the magnetic loop channeling model of particle beams.

Abstract

In this paper we present new results of spectraphotometrical investigations of the flaring kernels sizes and their intensities measured simultaneously in various parts of the H-alpha line profile. Our investigations were based on the very high temporal resolution spectral-imaging observations of the solar flares collected with Large Coronagraph (LC), Multi-channel Subtractive Double Pass Spectrograph and Solar Eclipse Coronal Imaging System (MSDP-SECIS) at Bialkow Observatory (University of Wroclaw, Poland). We have found that the areas of the investigated individual flaring kernels vary in time and in wavelengths as well as the intensities and areas of the H-alpha flaring kernels decreased systematically when observed in consecutive wavelengths toward the wings of the H-alpha line. Our result could be explained as an effect of the cone-shaped lower parts of the magnetic loops channeling high energy particle beams exciting chromospheric plasma.