Abstract
Magnetohydrodynamics (MHD) has proved very useful in describing the behaviour of space plasmas, in particular the solarwind flow around the Earth’s magnetosphere. The MHD flow problem is quite different from that in gasdynamics. This is because magnetic forces give rise to an asymmetric three-dimensional flow pattern. The structure of ideal MHD flowaround obstacles has a special features caused by a frozen-in magnetic field, even though this is relatively small in the ustream flow. The interplanetary magnetic field (IMF) is responsible for the boundary layer effects, which do not disappear regularly as the IMF is decreased.
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Erkaev, N.V., Farrugia, C.J., Biernat, H.K. (1998). Comparison of Gasdynamics and MHD Predictions for Magnetosheath Flow. In: Moen, J., Egeland, A., Lockwood, M. (eds) Polar Cap Boundary Phenomena. NATO ASI Series, vol 509. Springer, Dordrecht. https://doi.org/10.1007/978-94-011-5214-3_3
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