Other
Scientific paper
Jun 2006
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006spd....37.0822c&link_type=abstract
American Astronomical Society, SPD meeting #37, #8.22; Bulletin of the American Astronomical Society, Vol. 38, p.234
Other
Scientific paper
It is generally accepted that a large scale flux rope is a main constituent in solar eruptions, particularly in coronal mass ejections (CMEs) and filament eruptions. Although there are observations indicating emergence of twisted magnetic fields before some eruptive phenomena, the emerging field structures are usually much smaller scales than CME loops or erupting filaments. Large scale twisting (or shearing) motions are rarely observed and can hardly explain formation of eruption scale flux ropes. Our study is based on the assumption that the magnetic field below the solar surface consists of small scale filamentary flux tubes. These flux tubes are either already twisted before emergence or get twisted in the solar atmosphere by small scale vortical motions. The partitional structure of the magnetic field induces current sheets in the solar corona, and magnetic reconnection between the elementary flux tubes eventually takes place. However, the merging of line-tied flux ropes is not as straightforward as the merging of self-closed flux ropes in laboratory plasmas. Rather, the system stepwise goes through complex intermediate states comprising newly created flux ropes, which are longer than the original ones and wind around each other. The intermediate states evolve toward a simpler helical system of a larger scale as mutual helicities are transformed into self-helicity by magnetic reconnection. In this paper, the evolution of an idealized active region, which initially comprises small scale flux tubes, is followed by numerical simulation until a large scale erupting flux rope is generated and expelled beyond several solar radii. An observational example supporting our theory will also be presented.
Cheng C. Z.
Choe Gwang-Son
Lee Julian
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