Solar Eruptions Triggered by Flux Emergence
Abstract
Observations have shown a clear association of prominence eruptions and CMEs with the emergence of magnetic flux close to, or within, filament channels. It has been suggested that reconnection triggered by the emergence destroys the force balance between the magnetic field in the filament channel and its ambient field, causing the former to erupt. Magnetohydrodynamic (MHD) numerical simulations support this scenario for two-dimensional (2D) coronal flux-rope configurations. However, such simulations do not take into account 3D effects such as the anchoring of the flux rope in the dense photosphere or the occurrence of 3D MHD instabilities. Here we present the first 3D MHD simulations of (boundary-driven) flux emergence in the vicinity of a pre-existing coronal flux rope. We find that three processes are important for the evolution of the system: (1) expansion or contraction of the coronal field due to the intrusion of new flux, (2) reconnection between the emerging and pre-existing flux systems, and (3) repulsion or attraction of the respective current channels. We vary the position and orientation of the emerging flux and investigate under which conditions these processes can trigger an eruption.
- Publication:
-
AGU Fall Meeting Abstracts
- Pub Date:
- December 2019
- Bibcode:
- 2019AGUFMSH33B3390T
- Keywords:
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- 7509 Corona;
- SOLAR PHYSICS;
- ASTROPHYSICS;
- AND ASTRONOMY;
- 7513 Coronal mass ejections;
- SOLAR PHYSICS;
- ASTROPHYSICS;
- AND ASTRONOMY;
- 7524 Magnetic fields;
- SOLAR PHYSICS;
- ASTROPHYSICS;
- AND ASTRONOMY;
- 7959 Models;
- SPACE WEATHER