Comparison of the observed emission and the emission as synthesized from model. Left panel: emission of the AIA 171 Å channel of AR 12139 on 16 August 2014 at 23:30:48 UT near disk center. Right panel: synthesized emission of the same channel from the simulation as viewed from the top of the computation box. For better visibility, we use a nonlinear scaling of the images (power of 0.7 for the observation, and power of 0.4 for the synthesized emission). The color bars reflect this. The peak count value in the observations (corresponding to 1.00) is 3500 DN pixel−1; this is a factor of six lower for the model. This difference corresponds to a factor of 2.5 in density (see Sect. 5). The inlay shows a zoom-in of the region indicated by the white square. It shows a compact small loop. The color scaling is linear here. The observations and the model cover the same physical space on the Sun with a field of view of (515.9″)2 corresponding to (374.4 Mm)2. The numbers indicate the features discussed in Sect. 3. The blue dashed rectangle indicates the zoom-in used in Fig. 3.
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