Numerical Simulation of Solar Magnetic Flux Emergence Using the AMR–CESE–MHD Code

Magnetic flux emergence from the solar interior to atmosphere is believed be a key process of formation active regions and driving eruptions. Due limited capability observation, commonly studied using numerical simulations. In this paper, we developed model simulate twisted magnetic tube convection zone corona AMR--CESE--MHD code, which based on conservation-element solution-element method with adaptive mesh refinement. The result our simulation agrees that many previous ones similar initial conditions but different codes. early stage, rises as driven by buoyancy until it reaches close photosphere. decelerated there piling-up flux, instability triggered, allows field partially enter into atmosphere. Meanwhile, two gradually separated polarity concentration zones appear in photospheric layer, transporting energy through their vortical shearing motions. Correspondingly, coronal has also been reshaped sigmoid configuration containing thin current resembles typical pre-eruptive an region. Such framework established will applied future investigations how eruptions are initiated regions.