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Space-environment simulations, particularly those involving space plasma, present significant computational challenges. Global computational models based on magnetohydrodynamics equations are essential to understanding the solar system's plasma phenomena, including the large-scale solar corona, the solar wind's interaction with planetary magnetospheres, comets, and interstellar medium, and the initiation, structure, and evolution of solar eruptive events.
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Gombosi et al. (2004) studied this question.
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