Abstract
The role of the large- and medium-scale magnetospheric turbulence in the magnetospheric plasma dynamics is analyzed. The large scale convection electric field leads to plasma sheet compression which can be compensated by quasidiffusion flux directed against plasma pressure gradient. In the magnetostatic equilibrium regular and diffusion flux are compensated. On the basis of the developed theory the three dimensional solutions determining plasma sheet structure are modelled. The dependence of the plasma sheet structure on the interplanetary magnetic field (IMF) Bz orientation is investigated. It is shown that southward IMF orientation create the concave plasma sheet structure and northward IMF orientation can lead to the formation of convex structure in the center of plasma sheet. Possible explanation of theta-aurora formation is discussed.
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