on the estimation of scale-height of the disk we use, as in the case of NGC 3808B, only inner, most bright parts of profiles parallel to minor axis. The central region of the galaxy disturbed by the dust strip is also excluded. The values of scale-height are seen to increase while shifting from the galaxy nucleus, but not so much as in NGC 3808B: only 30%$-$50% for the distances from 5 kpc to 15 kpc from the nucleus.

As well as NGC 3808B, NGC 6286 demonstrates (see RC) both strong emission lines in circumnuclear region (within rectangular aperture $\rm 2.5"\times2.3"$ centered to the nucleus W(H$\alpha)\,=\,24\,\rm\AA$, $L$(H$\alpha)\,=\,2.1\,\times\,
10^{40}$ erg/s), and strong IR emission ($L\rm (FIR)\,\approx\,10^{11}$$L_{\sun}$). This may be a consequence of a burst of star formation induced by strong interaction with the companion. Emission-line spectrum of the nucleus is of HII-region type (RC).

### Forming ring

Photometric profile along the minor axis of the galaxy is shown in Fig.13a. The central part of the profile follows to exact exponential law. For $\rm r\geq$20" the main contribution to the observed brightness is given by the structure which we consider to be a ring forming around the galaxy. The ring is asymmetric: its 