The magnetosphere in the machine: Large scale theoretical models of the magnetosphere (95RG00397)

It has long been recognized that many of the macroscopic properties of the interaction of the solar wind with the magnetosphere can be understood by treating the solar wind as a fluid. For over thirty years gas dynamic models of the magnetosheath have been used successfully to model the position and shape of the bow shock and the plasma moments within the magnetosheath [Spreiter and Alksne, 1969]. In 1978 Leboeuf et al. [1978] developed the first global magnetohydrodynamic (MHD) simulation which modeled the magnetosphere as well as the magnetosheath self-consistently. Since then advances in computers and improved numerical techniques have helped us to build high resolution three dimensional models with which to investigate the configuration and dynamics of the entire solar wind, magnetosphere and ionosphere system.

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