Models of Arcade Flares in View of Observations by Yohkoh, SOHO/EIT and TRACE [Invited]

Details Models of Arcade Flares in View of Observations by Yohkoh, SOHO/EIT and TRACE [Invited] Models of Arcade Flares in View of Observations by Yohkoh, SOHO/EIT and TRACE [Invited]

Jan 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002mwoc.conf..181h&link_type=abstract

Multi-Wavelength Observations of Coronal Structure and Dynamics -- Yohkoh 10th Anniversary Meeting. Proceedings of the conferenc

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Scientific paper

Arcade formations in the arcade-type energy release phenomena suggest that there occur magnetic reconnections above the flaring arcades. On the other hand, dark filaments which suddenly erupt should play an important role in the energy release. Therefore a global model should explain the relationship between the dark filament eruption and the arcade flare in a consistent way. The idea that the dark filament is supported at the top of a simple loop and the magnetic reconnection occurs at the current sheet which is formed by the dark filament rise itself has been assumed in the "classical" model. But this model does not explain where the energy of the dark filament rise that breaks up the magnetic arcade comes from, and how the dark filament is supported at the top of a convex loop in a consistent way. Recent observations by Yohkoh, SoHO/EIT, and TRACE have revealed the magnetic configurations around dark filaments before the energy release, and suggest that the dark filament is supported in the neutral sheet between two magnetic loop systems with longitudinal magnetic field component along them, rather than supported on the top of a simple magnetic arcade. This fact is consistent with the quadruple magnetic source model of the dark filament. In the latter model, the strong part of the bipolar connections is opened up by the effect of the opposite polarity-pair of magnetic regions, and a current sheet exists before the event, in clear contrast to the "classical" model. The quadruple source model can explain the thin partition-type shape of dark filaments, and the presence of the barbs for the first time. MHD simulations based on this model show that the dark filament prevents the magnetic reconnection between the two magnetic loop systems until destabilized. As it is expelled out, the magnetic reconnection becomes possible, and the rise of the dark filament is accelerated upwards by the flood of upcoming magnetic flux through magnetic reconnection. These results of simulations can explain key observational features in very natural ways.

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