  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.
