Physics
Scientific paper
Dec 2005
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005agufmsh13a0294c&link_type=abstract
American Geophysical Union, Fall Meeting 2005, abstract #SH13A-0294
Physics
7509 Corona, 7513 Coronal Mass Ejections (2101), 7519 Flares, 7526 Magnetic Reconnection (2723, 7835)
Scientific paper
In eruptive flares with CMEs, several loop-shaped brightenings are often observed before the major mass ejection loop is ejected. The distance between the legs of the CME loop is generally much larger than the separation between H alpha flare ribbons or that between hard X-ray emission features. It can be thus inferred that the large scale erupting flux rope should be generated by reconnection among flux tubes that are commonly observed in the active region corona. These average scale flux tubes are energized by vortical motions, which are believed to be present in or below the solar surface and supply a net magnetic helicity to the coronal plasma system. In this 3D MHD simulation study, we follow the evolution of an idealized active region composed of several magnetic flux tubes whose original field connectivities are individually discrete. Vortical motions in the footpoint level are imposed within individual flux tubes so that the longitudinal magnetogram does not change at all while magnetic shear near the polarity inversion line rapidly increases as could be seen in a vector magnetogram of an eruptive active region. Magnetic reconnection between the flux tubes results in new field line connections, in which the distance between the footpoints is considerably larger than the original one. After a certain amount of magnetic flux is reconnected, a new helical flux rope of a visibly large scale is created and is expelled out of the active region leaving the underneath field lines open. An observational example corresponding to this simulation will also be presented.
Cheng C. Z.
Choe G.
Lee Julian
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