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Here is studied the presence of absorption components shifted to the violetor the red side of the main spectral line (satellite, or discrete absorptioncomponents, i.e. SACs or DACs), in Mg II resonance lines' regions in Be starsand their kinematical characteristics. Namely our objective is to check ifexists a common physical structure for the atmospheric regions creating SACs orDACs of the Mg II resonance lines. In order to do this, a statistical study ofthe Mg II {\lambda \lambda} 2792.523, 2802.698 {\AA} lines in the spectra of 64Be stars of all spectral subtypes and luminosity classes is performed. We foundthat the absorption atmospherical regions where the Mg II resonance linesoriginated may be formed of several independent density layers of matter whichrotate with different velocities. It is attempted also to separate SACs andDACs according to low or high radial velocity. The emission lines were detectedonly in the earliest and latest spectral subtypes.Comment: 18 pages, 12 figures, accepted for publication in PAS

The Complex Structure of the Mg II $\lambda\lambda$ 2795.523, 2802.698 ${\rmÅ}$ Regions of 64 Be Stars