MHD simulation for investigating the evolutionary path of a solar magnetic field that emerges, structures itself, erupts, and produces a flare

We performed a long-term magnetohydrodynamic simulation to reproduce the self-consistent evolution of a solar magnetic field, which comprises the initial phase when a magnetic flux tube emerges below the solar surface, the formation of a magnetic structure giving rise to a flux rope and sigmoid in the solar corona, and the final phase during which a flux rope erupts, followed by a flare with plasmoid ejection. By seamlessly reproducing dynamic processes involved in emergence, formation, eruption, and magnetic reconnection, we demonstrate the entire evolutionary path of an emerging flux tube leading to the onset of a flare.