First photometric study of three eclipsing binary star systems: V495 Aur, V589 Aur and V478 Cam

The light curve solutions and orbital period analysis of V495 Aur, V589 Aur and V478 Cam eclipsing binary star systems are presented for the first time in this study. Transiting Exoplanet Survey Satellite (TESS) observations were used as observational data. From the light curve solutions, it was concluded that all three systems are semi-detached binary star systems in which the secondary components fill their Roche lobes. The absolute parameters of the systems were also estimated. Accordingly, the photometric mass ratios of V495 Aur, V589 Aur and V478 Cam are found to be 0.251+/-0.035, 0.254+/-0.038 and 0.078+/-0.010, respectively. Upward parabolic change was observed in the O-C diagrams of all the systems considered. As a result of parabolic changes, we concluded that the orbital periods of the V495 Aur, V589 Aur and V478 Cam systems increased secularly with a rate of 0.050 +/- 0.010 s/year, 0.018 +/- 0.004 s/year and 0.070 +/- 0.015 s/year, respectively. The increases in orbital periods are explained by the dominant mass transfer mechanism from the secondary components to the primary components. In addition, the mass transfer rates between components and the rates of mass lost from the systems were estimated.