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This article proposes a picture of magnetized accretion structures formedduring the mass transfer in the Beta Lyrae system. It is shown that thestructure of the gaseous flows between the donor and the gainer is due to thespatial configuration of the donor magnetic field. Its dipole axis is deviatedsubstantially from the line joining the centers of the components and isinclined to the orbital plane of the binary system; the center of the magneticdipole is displaced from the donor center toward the gainer. The surface aroundthe donor magnetic pole, which is close to the gainer, is a region of anadditional matter loss from the donor surface. The effective collision of themagnetized plasma with the accretion disk is enhanced by the fastcounter-rotation of this disk, especially in the secondary quadrature phases,in which the high-temperature medium and the system of formed accretion flowsare observed. This concept is demonstrated, primarily, in the obviouscorrelations between the phase variability of the donor magnetic field and thecorresponding variability of the dynamic and energy characteristics of thevarious complex lines. This refers to the behavior of the radial velocitycurves of the emission-absorption lines formed in the gaseous structures oftype H$\alpha$, HeI $\lambda$ 7065, or the variability of their equivalentwidth and intensity, and the variability of conventional absorption lines ofthe donor atmosphere. This is true for the phase variability of the absoluteflux in the H$\alpha$ emission line and the fast varying of the continuum inthe H$\alpha$ region as certain parameters, which reflect the phase variabilityof the donor magnetic field. This approach made it possible to determine thephase boundaries of the location of the magnetic polar region on the donorsurface above which the matter outflows are formed.

Formation of magnetized spatial structures in the Beta Lyrae system II. Reflection of magnetically controlled structures in the visible spectrum