Data-driven modelling of solar coronal magnetic field evolution and eruptions

Graphical abstract

Magnetic fields play a fundamental role in the structures and dynamics of solar corona. As driven by their footpoint motions on the solar surface which transport energy from the interior of the Sun into its atmosphere, the coronal magnetic fields are stressed continuously with buildup of magnetic nonpotentiality in the form of topology complexity (magnetic helicity) and local electric currents (magnetic free energy). The accumulated nonpotentiality is often explosively released by solar eruptions manifested as solar flares and coronal mass ejections, during which magnetic energy is converted into mainly kinetic, thermal, and nonthermal energies of the plasma and could cause adverse space weather.