The depth and the vertical extent of the energy deposition layer in a medium-class solar flare. (arXiv:2009.06064v2 [astro-ph.SR] UPDATED)
<a href="http://arxiv.org/find/astro-ph/1/au:+Radziszewski_K/0/1/0/all/0/1">Krzysztof Radziszewski</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Falewicz_R/0/1/0/all/0/1">Robert Falewicz</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rudawy_P/0/1/0/all/0/1">Pawel Rudawy</a>
We analyze here variations of the position and the vertical extent of the
energy deposition layer (EDL) inthe C1.6 GOES-class solar flare observed at
10:20 UT on 2012 September 10. The variations of the EDL arecontrasted with the
variations of the spectra and emission intensities recorded in the H-alpha line
with the very high time resolution using the MSDP spectrograph at Bialkow
Observatory.
The flare radiated hard X-rays (HXR) detectable up to a energy of 70 keV. A
numerical model of the flare used in the analysis assumes that the non-thermal
electrons (NTEs) carried the external energy to the flare. The NTEs energy flux
was derived from a non-thermal component seen in RHESSI spectra. The main
geometrical parameters of the flare were derived using restored RHESSI imaging
data.
We found that the variations of the X-ray fluxes recorded in various energy
bands and the variations of the H-alpha intensities were well correlated in
time during the pre-impulsive and impulsive phases of the flare and they agreed
with the variations of the calculated position and vertical extent of the EDL.
The variations of the emission noticed in various parts of the H-alpha line
profile were caused by individual episodes of energy depositionby the beams of
NTEs of various energy spectra on various depths in the chromospheric plasma.
These results supplement our previous findings for the solar flare on 21
June2013, having nearly the same GOES-class of C1.1 but HXR emission below 34
keV only (Falewicz et al. 2017) (hereafter Paper I).
We analyze here variations of the position and the vertical extent of the
energy deposition layer (EDL) inthe C1.6 GOES-class solar flare observed at
10:20 UT on 2012 September 10. The variations of the EDL arecontrasted with the
variations of the spectra and emission intensities recorded in the H-alpha line
with the very high time resolution using the MSDP spectrograph at Bialkow
Observatory.
The flare radiated hard X-rays (HXR) detectable up to a energy of 70 keV. A
numerical model of the flare used in the analysis assumes that the non-thermal
electrons (NTEs) carried the external energy to the flare. The NTEs energy flux
was derived from a non-thermal component seen in RHESSI spectra. The main
geometrical parameters of the flare were derived using restored RHESSI imaging
data.
We found that the variations of the X-ray fluxes recorded in various energy
bands and the variations of the H-alpha intensities were well correlated in
time during the pre-impulsive and impulsive phases of the flare and they agreed
with the variations of the calculated position and vertical extent of the EDL.
The variations of the emission noticed in various parts of the H-alpha line
profile were caused by individual episodes of energy depositionby the beams of
NTEs of various energy spectra on various depths in the chromospheric plasma.
These results supplement our previous findings for the solar flare on 21
June2013, having nearly the same GOES-class of C1.1 but HXR emission below 34
keV only (Falewicz et al. 2017) (hereafter Paper I).
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