The Role of Reconnection in the Onset of Solar Eruptions

TL;DR

This study uses 3D MHD simulations to show that magnetic reconnection driven by the relative angle between emerging and pre-existing fields is crucial for triggering solar eruptions, highlighting a potential predictor for eruptive activity.

Contribution

It demonstrates that the relative angle between emerging and existing magnetic fields controls reconnection and eruption onset, emphasizing the importance of self-consistent modeling of the convection zone and corona.

Findings

Reconnection with overlying fields is essential for eruptions.

The relative angle determines the likelihood of eruption.

Eruptive behavior correlates with the amount of magnetic reconnection.

Abstract

Solar eruptive events such as coronal mass ejections and eruptive flares are frequently associated with the emergence of magnetic flux from the convection zone into the corona. We use three dimensional magnetohydrodynamic numerical simulations to study the interaction of coronal magnetic fields with emerging flux and determine the conditions that lead to eruptive activity. A simple parameter study is performed, varying the relative angle between emerging magnetic flux and a pre-existing coronal dipole field. We find that in all cases, the emergence results in a sheared magnetic arcade that transitions to a twisted coronal flux rope via low-lying magnetic reconnection. This structure, however, is constrained by its own outer field, and so is non-eruptive in the absence of reconnection with the overlying coronal field. The amount of this overlying reconnection is determined by the relative angle between the emerged and pre-existing fields. The reconnection between emerging and pre-existing fields is necessary to generate sufficient expansion of the emerging structure so that flare-like reconnection below the coronal flux rope becomes strong enough to trigger its release. Our results imply that the relative angle is the key parameter in determining whether the resultant active regions exhibit eruptive behavior, and is thus a potentially useful candidate for predicting eruptions in newly emerging active regions. More generally, our results demonstrate that the detailed interaction between the convection zone/photosphere and the corona must be calculated self-consistently in order to model solar eruptions accurately.