detected as pixels of WLF kernels in all flares on the the value of $\sigma_M$.[]{data-label="fig:sigma_spread"}](rozptyl.pdf){width="50.00000%"}

Results
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From the 54 WLF candidates the code detected an $I_{\rm c}$ emission in 25 cases. Interestingly, there does not seem to be a clear distinction of the flares with and without $I_{\rm c}$ emission as far as the flare class is concerned, both groups span over all investigated class range.

We investigated the dependence of the detected area (integrated in time) of the WLF ribbons on the flare intensity. It seems that there apparently are three different classes: a class (C0) without detected brightening in $I_{\rm c}$, the class (C1), where the number of detected kernel pixels is around 1000, and finally a class (CP), which seems to exhibit a power-law dependence of the number of kernel points on the flare intensity. All three are indicated in Fig. \[fig:classes\].

![Dependence of the total number of points in the WLF kernels on the flare strength. The dashed lines indicate the division of the flares into three classes mentioned in the text, they do not represent any fit of any kind.[]{data-label="fig:classes"}](pocetbodu_vs_tok_pro_sigma.pdf){width="70.00000%"}

![Example of the flare belonging to CP class. This X2.2-class flare ignited in NOAA 