Wei-Jie Hou(IANCU); Sheng-Peng Lan(IANCU); Li-Ching Huang(IANCU); Chia-Lung Lin(IANCU); Wing-Huen Ip(IANCU)
Because of magnetic activities, our Sun is characterized by the occurrence of sunspots and solar flares in an 11-year cycle. The frequency of large solar flares is correlated with the number of the sunspots and the source regions of the flares are generally co-located with the active regions near sunspots which are the storage sites of the magnetic energy. By the same token, the solar flare energy tends to be proportional to the size of the “source” sunspot in a statistical sense. One of the interesting results from the Kepler space telescope mission has to do with the discovery of the so-called superflares. From the Kepler measurements only the overall amplitudes of the light curve variations could be estimated even though it is highly desirable to know the sizes and size distribution of the star spots that might (or might not) be related to the superflares. As far as the analysis of the sizes of starspots is concerned, it has been proposed that the fine structures in the transit light curves due to the occultation effect of exoplanets could be used to resolve the star spot pattern with K 17 as the case in point (Desert et al., 2011; Valio et al., 2016). In this work, we will extend the study by Valio et al. (2016) to examine whether it is possible to derive the size frequency distribution and time variability of star spots from such high-precision photometric measurements. The future prospects are also discussed.