Forward modelling of brightness variations in Sun-like stars

The amplitude and morphology of light curves solar-like stars change substantially with increasing rotation rate: brightness variations get amplified become more regular, which has so far not been explained. We develop a modelling approach for calculating various rates use it to explain observed trends in stellar photometric variability. combine numerical simulations magnetic Flux Emergence And Transport (FEAT) model variability calculate synthetic as by the Kepler telescope. compute distribution flux on surface degrees active-region nesting (i.e., tendency active regions emerge vicinity recently emerged ones). Using resulting maps flux, we rotational our simulated function rate features compare calculations observations. show that both degree have strong impact curves. In order bulk \K{} targets known rates, need increase values much larger than Sun. suggested can provide clues emergence process high levels activity.