Abstract
Dynamics of the interaction of a magnetized supersonic plasma flow (solar wind) with a planetary ionosphere are examined. The flow behavior across a bow magnetohydrodynamic shock and in the post‐shock region, where the flow interacts with the planetary ionosphere, is analyzed. It is argued that the pressure balance between the solar wind and the post‐shock plasma is provided mainly by static gas pressure rather than by a large magnetic field ‘build‐up.’
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