The results obtained from the photometrical models are presented for KIC 2557430, which is known as an eclipsing binary system in the literature. Its light curve was analysed for the first time. The secondary component temperature was found as 6271±1 K. The mass ratio was computed as 0.868±0.002, while the inclination (i) of the system was found as 69 • .75±0 • .01. There is a third light contribution of 0.339% in the total light. 50 frequencies were found in the period analysis. 48 frequencies of them are caused due to the primary component, a γ Doradus star, while two of them are caused by the rotational modulation due to the cool spots. 69 flares were detected in the analyses. Two OPEA models were derived for these flares detected from KIC 2557430. Obtained OPEA models indicate that the flares were come from two different sources. The Plateau value was found to be 1.4336±0.1104 s for Source 1, which is seen as possible the secondary component and 0.7550±0.0677 s for Source 2, which is seen as possible third body. The half-life value was computed as 2278.1 s for Group 1 and 1811.2 s for Group 2. The flare frequency N1 was found to be 0.02726 h −1 and the flare frequency N2 was computed as 0.00002 for Group 1, while N1 was found to be 0.01977 h −1 and N2 was computed as 0.00001 for Group 2. As a result of this study, KIC 2557430 is a possible triple system. Considering both components' temperatures and obtained two different OPEA models, the primary star is a γ Doradus-type star, and the secondary component is a chromospherically active star, which has both the cool spot and flare activities, and also the third body, whose the membership status is controversial for this system, is a flare star.

We present new findings about KIC 8043961. We find the effective temperatures of the components as 6900 ± 200 K for the primary, and 6598 ± 200 K for the secondary, while the logarithm of the surface gravities are found to be 4.06 cm s-2 and 3.77 cm s-2, respectively. Combination of the light curve with the spectroscopic orbit model results leads to a mass ratio of 1.09 ± 0.07 with an orbital inclination of 73.71 ± 0.14 and a semi-major axis of 8.05 ± 0.22 R⨀ . Masses of the primary and secondary components are calculated as 1.379 ± 0.109 M⨀ and 1.513 ± 0.181 M⨀, while the radii are found to be 1.806 ± 0.084 R⨀ and 2.611 ± 0.059 R⨀. In addition, we obtain a considerable light contribution (≈0.54%) of a third body. We compute a possible mass for the third body as 0.778 ± 0.002 M⨀. We find that the primary component exhibits γ Dor type pulsations with 137 frequencies.