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We analyze here variations of the position and the vertical extent of theenergy deposition layer (EDL) inthe C1.6 GOES-class solar flare observed at10:20 UT on 2012 September 10. The variations of the EDL arecontrasted with thevariations of the spectra and emission intensities recorded in the H-alpha linewith the very high time resolution using the MSDP spectrograph at BialkowObservatory.  The flare radiated hard X-rays (HXR) detectable up to a energy of 70 keV. Anumerical model of the flare used in the analysis assumes that the non-thermalelectrons (NTEs) carried the external energy to the flare. The NTEs energy fluxwas derived from a non-thermal component seen in RHESSI spectra. The maingeometrical parameters of the flare were derived using restored RHESSI imagingdata.  We found that the variations of the X-ray fluxes recorded in various energybands and the variations of the H-alpha intensities were well correlated intime during the pre-impulsive and impulsive phases of the flare and they agreedwith 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 lineprofile were caused by individual episodes of energy depositionby the beams ofNTEs of various energy spectra on various depths in the chromospheric plasma.These results supplement our previous findings for the solar flare on 21June2013, having nearly the same GOES-class of C1.1 but HXR emission below 34keV only (Falewicz et al. 2017) (hereafter Paper I).

The depth and the vertical extent of the energy deposition layer in a medium-class solar flare