Abstract
The simplified description given by fluid models of magnetized plasmas makes it possible to simulate large scale problems such as the interaction of the solar wind with the earth's magnetic field. However, the accurate numerical solution of the fluid equations is made more difficult by the singular nature of the flow when magnetic reconnection occurs. During substorms, for example, details of small features of the flow in the magnetotail appear to cause changes in the global solutions. New methods for treating singular problems have been developed. Some of these are reviewed, including adaptive meshes and other tricks taken from fluid calculations. Several illustrative problems are described.
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Brackbill, J. Fluid modeling of magnetized plasmas. Space Sci Rev 42, 153–167 (1985). https://doi.org/10.1007/BF00218230
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DOI: https://doi.org/10.1007/BF00218230