  This article proposes a picture of magnetized accretion structures formed
during the mass transfer in the Beta Lyrae system. It is shown that the
structure of the gaseous flows between the donor and the gainer is due to the
spatial configuration of the donor magnetic field. Its dipole axis is deviated
substantially from the line joining the centers of the components and is
inclined to the orbital plane of the binary system; the center of the magnetic
dipole is displaced from the donor center toward the gainer. The surface around
the donor magnetic pole, which is close to the gainer, is a region of an
additional matter loss from the donor surface. The effective collision of the
magnetized plasma with the accretion disk is enhanced by the fast
counter-rotation of this disk, especially in the secondary quadrature phases,
in which the high-temperature medium and the system of formed accretion flows
are observed. This concept is demonstrated, primarily, in the obvious
correlations between the phase variability of the donor magnetic field and the
corresponding variability of the dynamic and energy characteristics of the
various complex lines. This refers to the behavior of the radial velocity
curves of the emission-absorption lines formed in the gaseous structures of
type H$\alpha$, HeI $\lambda$ 7065, or the variability of their equivalent
width and intensity, and the variability of conventional absorption lines of
the donor atmosphere. This is true for the phase variability of the absolute
flux in the H$\alpha$ emission line and the fast varying of the continuum in
the H$\alpha$ region as certain parameters, which reflect the phase variability
of the donor magnetic field. This approach made it possible to determine the
phase boundaries of the location of the magnetic polar region on the donor
surface above which the matter outflows are formed.
