MHD flow past an obstacle: Large‐scale flow in the magnetosheath

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Abstract
As a step to the study of the large‐scale flow in the magnetosheath, the MHD flow past an obstacle is investigated. A time asymptotic method is used to obtain 3D steady‐state solutions. The results indicate the formation of a depletion layer near the obstacle due to the increase of the magnetic field. Along the earth‐sun line the plasma density increases first and then decreases from the post bow shock to the magnetopause. The local density maximum in front of the magnetopause may correspond to what was recently observed. When the interplanetary magnetic field direction is tilted from the solar wind flow, the IMF influences the shape of the bow shock as well as the location of the stagnation point at the magnetopause in a way consistent with observation. In addition, the results show the existence of a magnetosheath current in the post parallel‐shock region.

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