of the galaxy. It means that interaction has to occur between gaseous disk of the galaxy and the ring. Therefore, if mass transfer from the companion stops then because of this interaction the ring structure must fall on the main galaxy disk very soon. Let us note also that inclined rings around spiral galaxies may be relatively stable only in the case when their diameters are larger than those of gaseous disks of main galaxies. ESO 235-58 (Buta & Crocker 1993) and NGC 660 (van Driel et al. 1995) are possible examples of such objects.

The formation of rings in NGC 3808B and NGC 6286 being accompanied by accretion of matter on galactic disks and interaction of two nearly orthogonal gaseous subsystems results in some interesting gasdynamical and stellardynamical effects in these galaxies. For instance, we may notice the peculiar rotation curve of NGC 3808B gaseous disk (see Fig.3b). Both galaxies demonstrate strong infra-red and H$\alpha$ emission pointing to the high star-forming activity. Stellar disks of both galaxies increase their thickness when going from the center to periphery and are bended in the outlying regions. One can conclude that double systems similar to those considered in this paper are unique 