both strong emission lines in circumnuclear regions (within rectangular aperture $\rm 2.5"\times2.3"$, centered on the nucleus, the equivalent width of H$\alpha$ emission line and the observed H$\alpha$ luminosity are found to be W(H$\alpha)\,=\,39\,\rm\AA$, $L$(H$\alpha)\,=\,2\,\times\,10^{40}$ erg/s) and intense far-infrared radiation ($L\rm (FIR)\,=\,4.4\,\times\,
10^{10}$$L_{\sun}$). For a sample of interacting galaxies Keel (1993) has found a correlation between H$\alpha$ equivalent width and greatest observed deviation from a symmetric rotation curve when normalized to the peak rotation velocity. Comparing the data for NGC 3808B with Fig.5 in Keel (1993) we find that the parameters of the galaxy are in agreement with the dependence presented in that paper.

To consider the problem of emission mechanism in the nucleus of NGC 3808B we compiled the results of spectral observations of the galaxy from Keel et al. (1985) and RC. The reddening was taken into account by standard way adopting $I$(H$\alpha$)/$I$(H$\beta$)$\,=\,$3.1 (Veilleux & Osterbrock 1987). The value of absorption in the direction of the nucleus was found to be $\rm 3.^{m}4$ in the $B$ band. It turned out that in standard classification diagrams ( \[O III\]$\lambda$5007/H$\beta$ vs. \[N II\]$\lambda$6583/H$\alpha$ and \[O I\]$\lambda$6300/H$\alpha$, one of these is given in Fig.7) reddening-corrected line ratios are located near the boundary 