Akademik Veri Yönetim Sistemi
New Astronomy, cilt.99, 2023 (SCI-Expanded)
© 2022 Elsevier B.V.By using different databases (TESS, SuperWASP, KWS and ASAS-SN), light curve analyzes of HX UMa and FP Boo systems were performed, and the changes in the orbital period of the systems were also examined. The light curve analyzes of the systems were conducted simultaneously with the radial velocities using the Wilson and Devinney (WD) code. As a result of the analyzes, the masses and radii of the components were determined as M1=1.29±0.02 M⊙, M2=0.38±0.02 M⊙, R1=1.21±0.02 R⊙, R2=0.78±0.02 R⊙ for HX UMa and M1=1.68±0.05 M⊙, M2=0.16±0.01 M⊙, R1=2.28±0.02 R⊙, R2=0.82±0.02 R⊙ for FP Boo, respectively. The distances of HX UMa and FP Boo were calculated as 123±11 pc and 350±23 pc, respectively, and were almost the same as Gaia DR3 values. When the orbital period changes were examined, it was determined that the orbital period of the HX UMa system increased, while the FP Boo decreased. The orbital period increase rate of HX UMa was calculated as dP/dt=9×10−8 d yr−1 and the period decrease rate of FP Boo was calculated as dP/dt=1.7×10−6 d yr−1. Mass transfer between components has been suggested as the reason for the period changes. Along with the orbital period changes, a cyclical change was observed in both systems. Magnetic activity or a possible third component can cause cyclical variation. The periods of these cyclical changes are determined as 24±4 yr and 20±1 yr, respectively.