“…In order to estimate F ν , the unsaturated SDO/AIA data were calibrated using the program aia_prep.pro and normalized to the exposure time for six EUV wavebands (94 Å, 131 Å, 171 Å, 193 Å, 211 Å, 335 Å). Then the differential emission measure [φ(T )] for the time interval 11:43:15 -11:43:27 UT was calculated from the area of a coronal source S c ≈ 4 × 10 18 cm 2 (Figure 7) corresponding to the 50% RHESSI contour (CLEAN algorithm, Hurford et al, 2002) in the energy range of 7 -10 keV based on the Tikhonov regularization technique (Tikhonov and Arsenin, 1979;Kontar et al, 2004Kontar et al, , 2005Hannah and Kontar, 2012;Motorina et al, 2012Motorina et al, , 2016. The results of numerical calculations of [φ(T )], averaged over the source area (Figure 8), show evidence that the coronal part of the flareenergy-release region contains a large amount of plasma with T = 0.5 -3 MK.…”