Exploring the solar paradigm to explain stellar variability

The unprecedented precision of broadband stellar photometry achieved with the planet-hunting missions CoRoT and $\mathit{\text{Kepler}}$ 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.