Abstract
This chapter describes the 3D Solar-Interplanetary space-time Conservation Element and Solution Element (SIP-CESE) MHD model and its application on the solar wind study. SIP-CESE MHD model is established on pentahedral cells with each cell a triangular prism composed of two triangular bases and three rectangular sides. The basic principle as well as the implementation detail of the CESE numerical scheme are presented. Two examples are given to illustrate the validity and capacity of modeling solar wind: (i) two-dimensional coronal dynamical structure with multipole magnetic fields and (ii) three-dimensional coronal dynamical structure, using measured solar surface magnetic fields and the empirical values of the plasma properties on the solar surface as the initial conditions for the set of MHD equations, and then the relaxation method to achieve a quasi-steady state. These examples show that the MHD model possesses the ability to model the Sun-Earth environment. Finally, the evolution of the large-scale coronal magnetic structure during solar cycle 23 is investigated by the SIP-CESE MHD model.
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