Determination of chromospheric activity indicators at the pulsation strip

In this thesis, it is tried to figure out the natures of KIC 2557430 and KIC 8043961, which were selected from the Kepler Database. For both systems, the pulsation frequency analyses were performed with PERIOD04 program. Examining the frequencies found from the analyses, it was found that both systems exhibit some variations caused by the pulsation and stellar spots. Light curve analysis was performed for both systems by PHOEBE V.0.32 software for the first time in the literature. In the case of KIC 2557430, it is seen that there is a third light excess as a result of light curve analysis. Considering the evolutionary status of the primary and secondary components of both systems depending on the parameters obtained from the light curves analyses, the primary component of KIC 2557430 was found to be a γ Dor type variable star. Examining the minimum time variations of both systems, it was suggested that there is a mass transfer from massive component to low mass component in the case of KIC 2557430. In the case of KIC 8043961, some signs were found for a third body. At the same time, 69 flares were obtained in total from the available data of KIC 2557430, and the parameters of these flares were calculated and modeled by the OPEA model. As a result of the model, it was found that the flares consist of two separate groups. From the spectral and frequency analyses of the KIC 8043961 system, it was determined that the system exhibits both the γ Dor and the δ Scuti type pulsations.