V381 Cas, V796 Cyg, and V871 Per are eccentric eclipsing binary systems exhibiting rapid apsidal motion. In this study, their light curves were analyzed for the first time using high-precision photometric data obtained from TESS observations. The photometric mass ratios were derived as q = 0.9294 ± 0.0007 for V381 Cas, q = 0.8146 ± 0.0030 for V796 Cyg, and q = 0.8854 ± 0.0027 for V871 Per. The (O – C) analyses were conducted by combining newly derived eclipse timings from TESS data with previously published minima. From these analyses, the apsidal motion periods were determined to be 20.45 ± 0.19 yr for V381 Cas, 32.55 ± 0.34 yr for V796 Cyg, and 70.80 ± 3.98 yr for V871 Per. Absolute parameters of the stellar components were also estimated. The masses of the components were calculated as follows: for V381 Cas, M1 = 2.06 ± 0.37, M⊙ and M2 = 1.92 ± 0.37, M⊙; for V796 Cyg, M1 = 3.31 ± 0.20, M⊙ and M2 = 2.70 ± 0.20, M⊙; and for V871 Per, M1 = 1.05 ± 0.14, M⊙ and M2 = 0.93 ± 0.14, M⊙. Furthermore, apsidal motion parameters were evaluated using both observational and theoretical internal structure constants ( and ). The relative contribution to the total apsidal motion rate was found to be less than 3% in all three systems.

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