Optical and EUV observation of a filament destabilization and pre-eruption reconnection

Details Optical and EUV observation of a filament destabilization and pre-eruption reconnection Optical and EUV observation of a filament destabilization and pre-eruption reconnection

Dec 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002esasp.506..573c&link_type=abstract

In: Solar variability: from core to outer frontiers. The 10th European Solar Physics Meeting, 9 - 14 September 2002, Prague, Cze

Physics

1

Filamets, Flare, Reconnection

Scientific paper

Filament eruption occurring prior to solar flares or CME may be related to changes in the magnetic field structure in and around the filament. In particular, when the magnetic field topology is characterized by great complexity, or new magnetic flux emerges in the surrouding of the main arcade supporting the filament, a so-called pre-eruption reconnection is likely to take place. In this framework, using both ground-based (THEMIS and BBSO) and satellite (TRACE) images and BBSO magnetograms, we have followed a filament eruption occurred in AR 9445 on May 5, 2001, before a two-ribbon flare. Our analysis has shown that the event was characterized by the following steps: a) presence of a knot of positive polarity inside the region of negative polarity where the arcade loops were anchored; b) appearance of a bright knot in Hα images at the same location where the positive polarity knot was observed; c) spread of the filament into two threads and bifurcation near the Hα bright knot; d) eruption of part of the filament and two-ribbon flare; e) EUV post-flare loops anchored in a region near the Hα bright knot. The interpretation of these phenomena in terms of a pre-eruption, low-lying magnetic reconnection, followed by a post-eruption, high-lying reconnection, is discussed.

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