NUMERICAL MODELLING OF THE SIZE AND TEMPERATURE VARIATIONS OF STAR SPOTS AND BRIGHT FACULAE OF MAGNETICALLY ACTIVE STARS FROM THE TRANSIT LIGHT CURVES

It is known that small-scale structures in the transit light curves of exoplanets can be used to infer the sizes and temperatures of dark spots or bright faculae of their host stars. Among many factors, the precision depends on the observational statistics, the ratio of the size of the exoplanet to that of the dark (or bright) spot and the cadence used in the light curve measurements. We have developed a numerical code allowing us to explore the effects and limitations of such a method for stars of different spectral types.