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tokens: software based on the analytical equation applied to spot modeling by Budding (1997) , assuming circular spots. Fixed parameters were the effective wavelengths of the filters used, linear limb darkening coefficients ( Howarth 2011 ) taking into account the stellar parameters, and the unspotted brightness in all bandpasses. We note that there is no way to deduce the true unspotted brightness of an active star showing the usual rotational and long-term light variations. On the other hand, one would expect a higher brightness level and smaller rotational variation with fewer and fewer spots. Therefore, we took the observed maximum magnitude as the unspotted reference brightness level. The rest of the activity is supposed to be distributed evenly and/or remain on the poles. We note that we have observed only two rotations of the star in a standard photometric system, and the archival and K2 data were obtained in different, non-standard bandpasses (except ASAS which has a V magnitude bandpass), and therefore cannot be compared quantitatively. We modeled in parallel the B − V , V − R C , V − I C color observations, assuming that there are just two circular starspots. The parallel modeling of each of these colors results in spot coordinates (longitudes, latitudes), sizes, and a single spot temperature. For EPIC 211759736 we have a high rotational inclination angle (81.85°), and thus the two stellar hemispheres are nearly interchangeable (supposing that the rotational axis is perpendicular to the orbit, the star is seen nearly edge-on), that is, approximately invariant under inversion. Therefore, in the course of the modeling, the spot latitudes were kept fixed at the equator; generally, it is not possible to obtain reliable spot latitudes from photometric data. In this way we had five free parameters to fit for: two longitudes and sizes, and the spot temperature. The results show that in early 2018 there were two cool spots (active regions) on the stellar surface, one facing the secondary component and the other on the opposite side, covering altogether about 10% of the total stellar surface, with a temperature of 3960 ± 300 K, or about 800 K below the surface temperature of 4750 K. The individual results of the spot temperature modeling from the three different color indices are as follows: B − V : 3968 ± 305, V − R C : 3936 ± 364, and V − I C : 3978 ± 215. Although the spot temperatures from the three color indices have substantial uncertainties, their values are remarkably close to each other. The resulting spot longitudes and sizes from the three color indices are within their mutual 1- σ uncertainties. The four-color light curves and the fitted color indices are plotted in Fig. 6 . (We note that experiments allowing the spots’ latitudes to also be free parameters gave essentially the same results for the longitudes, sizes, and temperature, but with much higher uncertainty due to the error propagation.) By contrast, the average stellar