Abstract
In this paper, we successfully use our newly developed numerical method to study the process of the emergence of magnetic flux rope from the solar convection zone into the atmosphere with a stratified hydro-static equilibrium as the initial ambient state. Our simulation has obtained some key characteristics revealed by observation or other researchers' simulations. To achieve the process from emergence until eruption requires a numerical scheme with low numerical diffusion. Otherwise, the emergence process will be suppressed by diffusion of magnetic flux during the long emergence period caused by the great gradient for density and pressure in the ambient state. The results demonstrate that our code can simulate the emergence process very well, which allows us to explore flux emergence mechanisms.
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