The Role of Magnetoconvection in the Evolution of Active Regions Before, During and After the Eruption of Coronal Mass Ejections

Details The Role of Magnetoconvection in the Evolution of Active Regions Before, During and After the Eruption of Coronal Mass Ejections The Role of Magnetoconvection in the Evolution of Active Regions Before, During and After the Eruption of Coronal Mass Ejections

Dec 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006agufmsh43b1529m&link_type=abstract

American Geophysical Union, Fall Meeting 2006, abstract #SH43B-1529

Mathematics

Logic

7509 Corona, 7513 Coronal Mass Ejections (2101), 7526 Magnetic Reconnection (2723, 7835), 7546 Transition Region, 7549 Ultraviolet Emissions

Scientific paper

We discuss the pre-eruptive evolution of an active region filament and the evolution of the ensuing post-eruptive "coronal dimming" based on observations of the EUV corona from the Solar and Heliospheric Observatory and the Transition Region and Coronal Explorer. We speculate that the erosion of coronal loop footpoints anchored in the weakest magnetic portions of an active region by magneto-convective flux emergence driven reconnection acts as a stochastic "tether cutting" mechanism. We discuss how this erosion of tethering magnetic flux is capable of creating a topological instability and eventual coronal mass ejection (CME) eruption. The magnetoconvection-driven magnetic reconnection and the global magnetic enviroment of the plasma are equally important in the "filling" and apparent motion of the region following the eruption of the CME. Further, we speculate that coronal dimmings could pose a potential secondary source of driving momentum to the CMEs that cause their initial appearance.

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