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Abstract:
Using the typical solar wind conditions during substorms, a series of numerical simulations based on a global magnetohydrodynamic(MHD) model are conducted to investigate the performance of the model on the comparison of its prediction with the in-situ observations from the spacecrafts. The results show that the model performs relatively well on the dayside of the magnetosphere, and the situation changes in the downstream region where a more sophisticated model is needed rather than the simplified MHD assumption. Among the eight physical variables, the magnetic field is the best approximated with a high correlation coefficient(CC) and prediction efficiency(PE), and the velocity takes the second. The modeled density and pressure have the relatively low CC and PE compared with the observation due to the limit of the MHD assumption for the solar wind, especially in the inner magnetosphere. Besides, the Dst index is modeled using an equavilent current approximation with the absence of a ring-current model. It is challenging to make a one-by-one comparison with the observation for the current MHD modelling in the magnetosphere.
