В работе представлены предварительные результаты анализа многоцветной BVRI фотометрии звезды MX Her. MX Her = TYC 3519-1418-1 является затменно-двойной системой типа Алголя с периодом обращения компонентов P = 2.3476536 дней, имеющей признаки пульсационной неустойчивости главной звезды. Наблюдения проводились в 2022 г. на телескопе Цейсс-600-Восточный, введенном в строй в том же году на обсерватории Майданак (Узбекистан) в рамках международного сотрудничества с Юннанскими обсерваториями (Китай). В настоящей работе впервые представлены решения многоцветных кривых блеска с помощью программы PHOEBE. В результате моделирования мы получили следующие оценки параметров системы: фотометрическое отношение масс системы M 2 /M 1 = 0.31, отношение эффективных температур T 2 /T 1 = 0.57, наклон орбиты i = 83.8 ◦ и эксцентриситет e = 0.0008. The paper presents preliminary results of the analysis of multicolored BVRI photometry of the MX Her star. MX Her = TYC 3519-1418-1 is an Algol-type eclipsing binary system with an orbital period P =2.3476536 days, showing signs of pulsational instability of the main star. The observations were carried out in 2022 on the ZEISS-600-East telescope, put into operation in the same year at the Maidanak Observatory (Uzbekistan) in the framework of international cooperation with the Yunnan Observatories (China). In this paper, solutions of multicolored light curves using the PHOEBE software are presented for the first time. As a result of the simulation, we obtained the following estimates of the system parameters: the photometric mass ratio of the system M 2 /M 1 = 0.31, the ratio of effective temperatures T 2 /T 1 = 0.57, the inclination of the orbit i = 83.8 ◦ and the eccentricity e = 0.0008.

We present the results of searching for new candidates of eclipsing binaries with eccentric orbits in the ASAS Catalog of Variable Stars (ACVS) using publicly available data from the All Sky Automated Survey (ASAS) and the Transiting Exoplanet Survey Satellite (TESS). Unsupervised machine learning techniques were applied to find anomalies among the light curves of eclipsing binaries. The light curves modeling were performed using JKTEBOP code. The pulsation analysis was done with FAMIAS. We identified 19 new eclipsing binary candidates with non-zero eccentricities in the ACVS, including 10 candidates with eccentricities e >= 0.1. Estimates of ec-centricities are given. We also report on possible presence of the small-amplitude stellar pulsations at least in two of the reported systems.

We describe here the formulation of our search for additional bodies in fifteen short period eclipsing binary stars and some results obtained by now. We intended to use two methods: transits across the surface of one or both stars (in order to detect planets) in the binary and a timing of eclipses of central binary stars (that can indicate the presence of a stellar mass body in the system). Observations were carried out using ground based photometry with 50-60 cm telescopes in 2013-2017. Until now no transits had been detected in our data. But at the same time we found several candidates for additional bodies in four systems. Further data processing will be performed.

AR CrB is a short-period low-mass eclipsing binary.We conducted photometric observations of the system in 2013, 2014, 2016, 2017, and obtained times of its light curves minima.The timing of eclipses (our times of minima combined with data from the literature) shows that the orbital period of AR CrB could possess periodical variations that can be explained by the gravitational influence of a third companion in a highly eccentric orbit around the central binary.

A short period eclipsing binary star CV Boo is tested for the possible existence of additional bodies in the system with a help of the light equation method. We use data on the moments of minima from the literature as well as from our observations during 2014 May–July. A variation of the CV Boo’s orbital period is found with a period of \({\approx}75~\mbox{d}\). This variation can be explained by the influence of a third star with a mass of \({\approx}0.4~\mbox{M}_{\odot}\) in an eccentric orbit with \(e\approx0.9\). A possibility that the orbital period changes on long time scales is discussed. The suggested tertiary companion is near the chaotic zone around the central binary, so CV Boo represents an interesting example to test its dynamical evolution. A list of 14 minima moments of the binary obtained from our observations is presented.