probably reflects large-scale rotation of the forming ring. From simple geometrical arguments used earlier for NGC 3808B, we have found that active phase of interaction between the galaxies being accompanied by mass transfer has been lasting no more than $\rm 5\times10^{8}$ years.

Conclusions
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In this work we give the results of observations of two spiral galaxies in close interacting systems. In both systems mass transfer from one galaxy to another is observed, accreting matter forming large-scale ring-like structures rotating around the major axes of considered galaxies. Because of existence of two kinematically distinct subsystems rotating in orthogonal planes these objects - NGC 3808B and NGC 6286 - look very much like polar-ring galaxies. Both galaxies clearly illustrate the possibility that PRGs may be formed as a result of matter accretion from one galaxy to another (Schweizer et al. 1983).

In NGC 6286 the ring structure seems to be at relatively earlier stage of formation than in NGC 3808B. Accreting matter in NGC 6286 probably did not have time to perform the whole revolution around the galaxy.

Both galaxies with forming rings are spirals and in both cases the diameter of observed ring is comparable (or even smaller) with diameter 