  The unprecedented precision of broadband stellar photometry achieved with the
planet-hunting missions CoRoT and \textit{Kepler} initiated a new era in
examining the magnetically-driven brightness variations of hundreds of
thousands of stars. Such brightness variations are well studied and understood
for the Sun. The plethora of data allows to accurately compare solar and
stellar brightness variations. An intriguing question is whether the observed
trends in the stellar photometric variability (e.g. the dependence of the
variability on the stellar rotation period) can be explained by utilising the
solar paradigm, in particular the physical concepts of brightness variations
learnt from the Sun. The goal of this work is to find out, through comparison
of observational and simulated data, if any physical concepts of solar
brightness variability have to be altered to reproduce the distribution of
Sun-like stars variabilities.
