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This study depends on KIC 9641031 eclipsing binary system with achromospherically active component. There are three type variations, such asgeometrical variations due to eclipses, sinusoidal variations due to therotational modulations and also flares, in the light curves obtained with thedata taken from the Kepler Mission Database. Taking into account resultsobtained from KIC 9641031's observations in the Kepler Mission Database, wepresent and discuss the details of chromospheric activity. The sinusoidal lightvariations due to rotational modulation and the flare events were modelledseparately. 92 different data subsets separated using the analytic modelsdescribed in the literature were modelled separately to obtain the cool spotconfiguration. It is seen that just one component of the system ischromospherically active star. On this component, there are two active regionsseparated by about 180 deg longitudinally between the latitudes of +50 deg and+100 deg, whose locations and forms are rapidly changing in short timeintervals. 240 flares were detected and their parameters were computed. Usingthese parameters, the One Phase Exponential Association (hereafter OPEA)function model was derived, in which the Plateau value as a saturation level ofthe flare-equivalent duration was found to be 1.232 s for KIC 9641031, andhalf-life parameter was found to be 2291.7 s. The flare frequency N1 was foundto be 0.41632 h-1, while the flare frequency N2 was found to be 0.00027.Considering these parameters together with the orbital period variationsdemonstrates that the period variations directly depend on chromosphericactivity. Comparing the system with its analogue it is seen that the activitylevel of KIC 9641031 is remarkablely lower than the others.

Detailed Chromospheric Activity Nature of KIC 9641031