Close binary systems in multiple stars: III. Eclipsing variables with LITE effect

The list of 240 eclipsing variables with the light equation (LITE effect) has been compiled. Some characteristics of multiple systems have been determined assuming that those stars may contain extra components. Quantity distributions have been obtained for Close Binary Systems (CBSs) with LITE effect and for those without it. The observed excess of short period stars (<0.3 days) is shown to be realistic. The eccentricities of Long Periodic Orbits (LPOs) have a parabolic distribution with a weak maximum at e = 0.28. The ratios of LPO to CBS periods cannot be considered to be random. The dependence of those values on LPO periods has been revealed. The distributions of periods and semimajor axes of LPOs are shown to have maxima at P 3 = 32 yrs and a = 16 AU, respectively. The latter distribution can be described by the Gaussian function. Approximately 85% of tertiary companions in stellar systems have a mass which is half as much as the total CBS mass. Except for one CBS (RR Lyn), all multiple systems of the obtained list are dynamically stable configurations. The possibilities to detect tertiary companions using speckle interferometry observations and proper motions of CBSs, as well as by extra light contribution when analyzing light curves and radial velocity changes of the CBS center of mass are discussed. Other causes are considered which may be a reason for the LITE effect, such as the mass exchange in CBSs and the influence of the magnetic field of components. Certain difficulties may arise when interpreting the LITE effect caused by the magnetic field of components. The most promising research directions in detecting tertiary companions in CBSs with the LITE effect are suggested.

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