Callebaut, Dirk K.Karugila, Geoffrey K.Makarov, Valentin I.2023-03-222023-03-222004http://www.suaire.sua.ac.tz/handle/123456789/5066Journal articleThe E × B drift allows plasma to move through the magnetic field lines and may contribute to various motions inside the Sun (e.g. to explain the adverse gradient of differential rotation in the equatorial zone), at its surface and in the corona. Here we treat an example: using a given azimuthal angular frequency ω(r, θ), rather arbitrary, and the corresponding exact solution for B, we obtain E and the drift velocity. The latter is comparable with the original velocity, but has components in all directionsenMagnetohydrodynamics (MHD)Convective zoneE × B driftArticle