Astronomy and Astrophysics – Astronomy
Scientific paper
May 2007
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007aas...210.2915c&link_type=abstract
American Astronomical Society Meeting 210, #29.15; Bulletin of the American Astronomical Society, Vol. 39, p.139
Astronomy and Astrophysics
Astronomy
Scientific paper
Structures observed in the solar atmosphere are generally of smaller scales than those structures that are observed in solar eruptions, such as CME loops and erupting prominences. Although an eruption intrinsically involves a volume expansion of the structure to erupt, there is observational evidence that the erupting structure forms by interaction and merging of smaller scale structures in steps. In this paper, the evolution of an idealized solar active region composed of a number of flux tubes is investigated by three dimensional magnetohydrodynamic simulations. Under low electrical resistivity as in the solar atmosphere, the partitional structure of the active region magnetic field is not readily destroyed. Thus, the corrosion of the current sheets, which partition individual flux systems, proceeds slowly but continuously until a rather fast magnetic reconnection process abruptly changes the global topology of the system. However, a total merging of the cellular flux systems cannot be achieved all at once. The system evolves into intermediate stages, which consist of cellular flux systems of incrementally larger sizes. An eruptive phase eventually sets in when partitional flux systems are fused to form a highly self-wound magnetic structure of the largest scale. A relevant observation will be presented with simulation results.
This work was supported by NASA grant NNH04AA16I.
Choe Gwang-Son
Lee Julian
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