distribution for $\rm r\le20"$ are $h\,=\rm\,3.9"\pm0.35"$ (exponential scale-length) and $\mu_{0}(V)\,=\rm\,18.5\pm0.2$ (central surface brightness). After transforming $\mu_{0}(V)$ value to $\mu_{0}(R)$ (in the Cousins system) by assuming that $V-R\,=\,$0.5 we have compared the disk parameters of NGC 3808B with those for large sample of interacting galaxies studied in Reshetnikov et al. (1993b). The photometric parameters of NGC 3808B are found to be typical for extremly interacting galaxies (Figs.13 and 15 in cited paper).

It is well known that in normal spirals the z-structure of stellar disks is well represented by the model of a locally isothermal, self-gravitating stellar sheet with scale-height $z_{0}$ independent on galactocentric distance (van der Kruit & Searle 1981). The disks of non-dwarf spiral galaxies can be characterized by the value of $z_{0}\,=\rm\,0.7\pm0.2$ kpc (van der Kruit 1989). The distributions of $z_{0}$ values along the disk of NGC 3808B in three passbands are given in Fig.5. To eliminate the influence of twined arm and surrounding envelope, only the most bright inner parts of profiles parallel to the minor axis were used for estimating the scale-height values of the disk. As one can see, these values increase with moving away from the center of galaxy (at the edge of the 