Abstract
We have investigated how a weak radial magnetic field (B 0 ∼10 G) influences the dynamics in the equatorial plane of the envelopes of Be stars. We calculate the distributions of the azimuthal velocity and the azimuthal magnetic field for models with various mass-loss rates, radial velocity distributions, and strengths of the radial component of the magnetic field at the surface of the star. Our investigation has shown that, in a slowly expanding envelope, a weak magnetic field can influence the rotational velocity distribution quite effectively by transferring angular momentum from the magnetic field to the material
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