Timing of eclipsing binary V0873 Per: a third body candidate

Abstract

We analyse a set of moments of minima of eclipsing variable V0873 Per. V0873 Per is a short period low mass binary star. Data about moments of minima of V0873 Per were taken from literature and our observations during 2013-2014. Our aim is to test the system on existence of new bodies using timing of minima of eclipses. We found the periodical variation of orbital period of V0873 Per. This variation can be explained by the gravitational influence of a third companion on the central binary star. The mass of third body candidate is $\approx 0.2 M_{\odot}$, its orbital period is $\approx 300$ days. The paper also includes a table with moments of minima calculated from our observations which can be used in future investigations of V0873 Per.Comment: 8 pages, 5 figures, 4 tables, accepted for publication in Astrophysics and Space Scienc

Magnetic Activity on Four Short-period Contact Binaries: V0576 Peg, KW Psc, V0873 Per, and FY Boo

“…The observed times of minimum light from 2007 to 2021 cover the whole period of P mod = 10.8(±0.1) yr. The previously published results (Krwittanawong & Poojon 2015;Bogomazov et al 2016) may result from only the 7 yr observations from 2007 to 2014, mainly to fit two scattered points, i.e., HJD 2,455,497.6874 (Diethelm 2010) andHJD 2,455,484.9228 (Diethelm 2011a). Our result implies that those two data do not lie around the general trend.…”

“…The semiamplitude of cyclic variation is only A = 0 0010(2). After neglecting the epoch time mentioned above, Bogomazov et al (2016) removed the period decreasing and derived another 300-day oscillation. These inconsistent results may originate from a short span of observations.…”

“…They also suggested that its orbital period may be decreasing, overlaying a 4 yr cyclic oscillation with a low amplitude of 0.0010(2) days. Meanwhile, Bogomazov et al (2016) derived another period variation with a period of ∼300 days.…”

A possible additional body in eclipsing binary system HS 2231+2441

“…Из их сравнения определяются неизвестные параметры светового уравнения (О-С). Так называемый метод тайминга основан на регистрации вариаций периода какого-либо периодического процесса, связанного со звездой [3,6,8,9]. Исследование звездной затменно-двойной системы в течение длительного времени позволяет получить серию из нескольких транзитов, зависящих от орбитального периода меньшего спутника.…”