On the Eruptivity of the Magnetic Field in Data-driven Time-dependent Coronal Simulations

Accurate characterization of the magnetic field via modeling is of key importance for advancing our understanding of the formation and dynamics of eruption-prone structures in the corona. While non-linear force-free extrapolations provide a snapshot in time of the topology of the low-coronal magnetic field, their value in determining the stability of the field is limited. Time-dependent modelling, on the other hand, offers a promising path to model the evolution of the coronal magnetic field and thereby advance beyond the current paradigm of static extrapolations.

In this work, we present results of our time-dependent magnetofrictional simulations of the evolution of active region magnetic fields. The model is driven by the photospheric electric field inverted from a time-sequence of HMI vector magnetograms. Using our experience from modeling several active regions, we discuss the conditions that lead to the formation of eruptive structures. In particular, we focus on understanding how the energy and helicity injected from the photosphere distributes in the corona to form structures that are prone to erupt.