Data-Constrained Modeling of Eruptions in the Solar Corona: Insights from 3D MHD Simulations

Understanding the energy storage and release processes of solar eruptions, also known as Coronal Mass Ejections (CMEs), remains challenging on multiple fronts. On one hand, the complexity of solar active regions, and the myriad ways in which they present themselves, makes it difficult to pin down the essential mechanisms of CMEs. On the other hand, our primary way of observing the early stages of CMEs is through remote sensing diagnostics, which provide only partial inferences of the underlying plasma state. Sophisticated models that capture both the energy storage and release processes in tandem with remote sensing diagnostics are one way to approach this problem. Using these ideas to frame our discussion, we present an overview of the essential steps for constructing a case-study, data-constrained model of a solar eruption using a 3D thermodynamic MHD model of the global solar corona. Choices for boundary conditions, energy storage, initiation, and the global coronal background all have significant consequences for the ensuing evolution and interpretation of results. Despite these complexities and challenges, we show how such modeling can be used to directly connect the observable consequences of CMEs (EUV waves, coronal dimming) to their underlying physical processes (CME expansion and connectivity changes). Such modeling helps to unify our picture of CMEs as they evolve and interact with disparate regions of the solar atmosphere. Future prospects will also be discussed.