The simulation of the coronal mass ejection-shock system in the inner corona

In the concept that coronal mass ejections (CME) are usually originated in large closed magnetic field regions which are found in the coronal streamer belt near the solar surface, we have used a thermal driving force so stron g that portions of the closed magnetic fields were carried away by the stro ng disturbance. A CME-shock system is obtained in the inner corona. The "le gs" of loop-like CMEs are again obtained at the interface between the coron al open and closed magnetic fields. However, there is no counterpart in out er space. The shock is a combined one with an intermediate shock near the e quator at its early stage. Ultimately, it becomes a pure fast shock. A plas moid with higher density and bubble-like magnetic fields is formed behind t he MHD shock wave. It propagates at high speed. The results show that the h igh-speed plasmoid does not propel the MHD shock in front of it; rather, th e plasmoid forms behind die MHD shock.