emission, in favour of the backwarming model.

It has to be noted that indications for flares in the white light were also observed on other stars, first on young or magnetically interacting stars, such as the RS CVn type, and magnetically active M dwarfs. Flares on Sun-like stars were not seen until the availability of the high-cadence high-precision photometry [@2000ApJ...529.1026S]. Recently [@2012Natur.485..478M] reported on observations of large-energy flares on Sun-like stars recorded in the [*Kepler*]{} light curves. In general, it is believed that the most important contribution to flares observed in the range of the visible light on other stars comes from the Paschen continuum [e.g. @2006ApJ...644..484A]. The appearance of the flares is not reserved to only stars of a late spectral type, but apparently also to hotter stars of type A [e.g. @2012MNRAS.423.3420B; @2016ApJ...831....9S], however recent observations do no confirm this idea [@2017MNRAS.466.3060P].

The aim of our study is twofold. First, we develop a code that allows a detection of brightenings in the intensity images that have properties of WLF kernels. We describe the algorithm behind our code, properly determine the values of tunable parameters and test it. Second, we show a rather simplistic application to the results returned 