Abstract
In the paper results for modelling a characteristic pattern of the solar wind flow and its turbulent structure are presented. We use a gravitational magnetic hydrodynamic model, and for the model we have created an effective numerical method based on Godunov’s method and piecewise parabolic reconstruction of the solution. We consider the evolution of the MHD turbulence of the supersonic gas flow, where random strong transversal velocity disturbances are set, the problem is considered in the vertical magnetic field. For the formation of a reference test of the supersonic MHD turbulence evolution a detailed analysis of the flow is carried out.
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