Abstract
In our research, we have studied 6 close binary stellar systems which are
eclipsing variables of $\beta$ Lyrae and W Ursae Majoris types of variability.
We have studied their O-C curves. To build them, we used moments of minima,
listed in the BRNO database. Also, we used ones, which we obtained as the
result of processing of observational data taken from AAVSO database. As the
result of the O-C analysis, we detected that all of these stars have parabolic
O-C curves, which might be caused by mass transfer from one component to
another. In an addition, 3 from researched stars (U Peg, V0523 Cas and WZ Cyg)
have superimposed parabolic and cyclic O-C changes that could be caused by
presence of the third components in the systems. Also, we calculated minimal
possible masses of third components, rates of the mass transfer for these
systems and corrected the ephemerides.
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