of current sheets is expected. This finding is in agreement with models of magnetic reconnection in flares. In the high-tail range, the histograms of C1 and CP are not different, as the according to the Kolmogorov-Smirnof test, there is a 71% probability that the apparent differences are due to chance. On the other hand C1 and CP histograms differ significantly in the low-values range, where for the CP-class flares the $f$ values seem to be significantly larger with a level of a statistical significance better than 99%.

It is not surprising that the histogram curves of $f$ in the C1 and CP regions lie below both curves in large-values range and in between in a smaller-values range, as it contains the information about the magnetic field gradients of both classes combined. On the other hand, the histogram of magnetic field gradients is somewhat surprising for the class C0, which seems quite similar as the histogram for CP class, despite the fact that according to the Kolmogorov-Smirnof test, they are strictly different. It might be that in C0 group the reason for non-detection of the VL emission is purely technical and that with a lower threshold in the code the VL 