First photometric study of a short-period detached eclipsing binary NSVS 10441882

Abstract NSVS 10441882 is a newly discovered eclipsing binary system with strong magnetic activity and an orbital period of  ∼ 0.5166 days. In order to study this eclipsing binary system, we analyzed its first four-color ( BVR c I c ) light curves. The observed light curves were asymmetric, so we used the 2013 version of the Wilson–Devinney (W–D) program with cool star-spots to analyze these data. We discovered that NSVS 10441882 is a detached total eclipsing binary system with an orbit inclination of 85°.34  ± 0.07 and a mass ratio of q  = 0.94  ± 0.03. Based on the CCD times of the light minima according to our observations and those reported previously, the orbital period changes of NSVS 10441882 were studied using the traditional O–C method for the first time. The O–C diagram of the target exhibited a cyclic oscillation with a period of 16.7  ± 0.20 years and an amplitude of 0.00349  ± 0.00029 days, probably due to the presence of an unseen third body. If we assume that the total mass of NSVS 10441882 is 1.3M ⊙ (according to our calculated results for the average color index and mass ratio), then the mass of the third body is no less than 0.12  ± 0.01 M ⊙ . Moreover, the orbital evolution of the central system will be accelerated due to the presence of this additional component.