Abstract:
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 Hα,
He I λ 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 Hα emission line and the fast varying of the
continuum in the Hα 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.
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