A selection of eclipsing variables was made from the sixth catalogue of orbits of visual binary stars. The obtained list of variables was supplemented with physical parameters and some orbital elements of triple stars. The histogram of angles between orbital planes of close and wide pairs was constructed. It is shown that in 2/3 cases these angles do not exceed 20° and the difference of the angles increases with the enhancement of the major semi-axis of a visual orbit. The distribution of the long and short period ratios has local maxima at some intervals. The dynamical sum of masses of triple systems and sums of masses of close binaries which were found through precise methods and masses of tertiary components obtained using the mass-luminosity relation are in good agreement. Masses for most of tertiary components are two times less than ones for close pairs. Precession periods of close binary orbit planes were estimated to be between some thousand and some ten million years.