  Here is studied the presence of absorption components shifted to the violet
or the red side of the main spectral line (satellite, or discrete absorption
components, i.e. SACs or DACs), in Mg II resonance lines' regions in Be stars
and their kinematical characteristics. Namely our objective is to check if
exists a common physical structure for the atmospheric regions creating SACs or
DACs of the Mg II resonance lines. In order to do this, a statistical study of
the Mg II {\lambda \lambda} 2792.523, 2802.698 {\AA} lines in the spectra of 64
Be stars of all spectral subtypes and luminosity classes is performed. We found
that the absorption atmospherical regions where the Mg II resonance lines
originated may be formed of several independent density layers of matter which
rotate with different velocities. It is attempted also to separate SACs and
DACs according to low or high radial velocity. The emission lines were detected
only in the earliest and latest spectral subtypes.
