Astronomy and Astrophysics – Astronomy
Scientific paper
Jun 2009
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009apj...697..999l&link_type=abstract
The Astrophysical Journal, Volume 697, Issue 2, pp. 999-1009 (2009).
Astronomy and Astrophysics
Astronomy
8
Sun: Filaments, Sun: Flares, Sun: X-Rays, Gamma Rays
Scientific paper
We present an observational study on the impact of the dynamic evolution of kinking filaments on the production of hard X-ray (HXR) emission. The investigation of two kinking-filament events in this paper, occurring on 2003 June 12 and 2004 November 10, respectively, combined with our earlier study on the failed filament eruption of 2002 May 27, suggests that two distinct processes take place during the kink evolution, leading to HXR emission with different morphological connections to the overall magnetic configuration. The first phase of the evolution (Phase I) is characterized by compact HXR footpoint sources at the endpoints of the filament, and the second phase (Phase II) by a ribbon-like footpoint emission extending along the endpoints of the filament. The HXR emission in both the 2002 May 27 and 2004 November 10 events shows a transition from Phase I to Phase II. In the 2002 May 27 event, coronal emission was observed to be associated with EUV brightening sheaths aligned along two filament legs in Phase I, while in Phase II, it was located near the projected crossing point of the kink. The coronal emission in the 2004 November 10 event does not exhibit a clear morphological transition as in the 2002 May 27 event, probably due to the filament's relatively small size. The 2003 June 12 event mostly features a Phase I emission, with a compact footpoint emission located at one end of the filament, and an elongated coronal source oriented along the same filament leg. We propose the following scenarios to explain the different flare morphology: magnetic reconnection in Phase I occurs as a result of the interactions of the two writhing filament legs; reconnection in Phase II occurs at an X-type magnetic topology beneath the filament arch when the filament ascends and expands.
Alexander David
Liu Rui
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