The magnetic boundary layer of the Earth as an energy-supplying channel for the processes inside the magnetosphere

Quasi-viscous interaction between the solar wind plasma and the geomagnetic field regularly takes place at the boundary of the magnetosphere. Like the effect of reconnection of force lines of the Earth magnetic field and the interplanetary magnetic field (IMF) transported by the solar wind the intensity of the quasi-viscous interaction depends on the magnetic viscosity of the plasma. Anomalous increase of the value of this parameter in the MHD boundary layer of the Earth, the magnetopause is analogized with which, is connected with the variation of the solar wind perturbation. In such circumstances for presenting the development process of the magnetopause dynamics the numerical and analytical methods of mathematical modeling have been used. Their effectiveness depends on the quality of the model describing the energy transmission process from the solar wind to the magnetopause. Usually, adequacy of a model for the development dynamics of the phenomena inside the magnetosphere is assessed in this way. In this work one of such theoretical models is considered. This model is based on the Zhigulev “magnetic” equation of the MHD boundary layer, which is simplified by means of the Parker velocities kinematic model. In order to clearly show the physical mechanisms stipulating the energy transmission process from the magnetosphere boundary to its inner structures some new characteristics of the MHD boundary layers are presented: thicknesses of magnetic field induction and the energy driven into the magnetopause. Besides, in the magnetic field induction equation several models of impulsive time variation of the magnetic viscosity of the solar wind is used and by means of the sequent approximation method an analytical image of quasi-stationary variation of the magnetopause parameters correspondent to these models is presented.