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 selfconsistent
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.
Reference
Magara, Tetsuya
Publication of Astronomical Society of Japan, 67, L6