Magnetohydrodynamic models of the upper atmosphere of Earth and some applications thereof

The earlier developed monotonous conservative variant of a net-characteristic method of the second- and third-order approximation based on 3D equations of magnetic gasodynamics with consideration for the magnetic field diffusion is expanded for the solution of dynamic problems on the flow of the upper atmosphere of the Earth by solar plasma. It is modified, which results in support for the solenoidality of the magnetic field and the removal of the magnetic charge. Calculations are carried out and preliminary results of using software complexes to simulate the passage of the leading edge of solar plasma through the upper atmosphere of the Earth are given. Unlike existing studies in this direction, the dynamics of the passage of the leading edge upon a strong burst in the intensity of solar wind over the entire altitude range from the surface of the Earth to the upper magnetosphere is considered.