Solar eruption is the most violent energy release process and active phenomena in the solar atmosphere, its main manifestation styles include solar flare, eruptive prominence, coronal mass ejection (CME) and so on. Because of the motion of photospheric plasma and magnetic flux emergence, magnetic energy is transformed continuously from the region below the photosphere to the corona, and stored in the complex coronal magnetic structure eventually. When these magnetic energy stored in the corona be accumulated to a certain extent, the whole magnetic structure will suffer catastrophic changes due to the joining of various plasma instabilities, release lots of magnetic energy, heat ambient plasma and accelerates high energy particles. In a typical solar eruption, for example a CME/flare event, it usually be accompanied by plenty of observational phenomena; the global wave phenomena and magnetic reconnection process are two important members among them.In order to investigate the solar eruption and accompanied phenomena, we perform detailed simulations under the support of NIRVANA which aims to solve the MHD problems in the astronomical environment, based on the widely accepted flux-rope model for the solar eruption. The magnetic structure of flux rope model includes a current carried rope to model the prominence floating in the corona, its inducted image because of the conductive photosphere surface, a force-free background field being used to confine the rope and the CS formed during eruption due to the idea MHD environment.
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