thus compensate for Doppler shifts of the line core . The H$\alpha$ image is relatively unchanged, while the other images are more affected. This difference is caused by the large thermal broadening of H$\alpha$ compared to the other lines, which makes it less sensitive to Doppler motions. In the and lines the carpet of fibrils now appears thicker and sharper than in the nominal line-core images. The flare ribbons are now visible in these lines, even in  8542 Å.

The simulated images exhibit features that quite resemble observational features in our Fig. \[fig:observations\] or Fig. 1 by @2011ApJ...742..119R. The observations show that [K]{} and H$\alpha$ trace roughly the same structures. The  8542 Å often shows different fibrils, with more visible patterns of waves and shocks from the lower chromosphere.

The SST/CRISP, SST/CROMIS, and, to a lesser extent, IRIS observations show finer structures than the synthetic images. This is most likely caused by the finite horizontal grid spacing (96 km) of the model atmosphere compared to the resolution of the observations ($\sim$100 km for SST, $\sim$250 km for IRIS). showed for radiation-MHD models of the enhanced network that synthetic fibrils get thinner and closer in appearance to the observed ones if 