Study of solar flares and filament interaction in NOAA 10501 on 20 November, 2003

R. Chandra1*,B. Schmieder2, C. H. Mandrini3, P. Démoulin2, E. Pariat2, T. Török4 ,G. Aulanier2 ,W. Uddin5 and M. G. Linton6
1Department of Physics, DSB Campus, Kumaun University, Nainital, India- 263 002
2LESIA, Observatoire de Paris, 92190 Meudon, France
3Instituto de Astronomía y Física del Espacio (IAFE), CONICET-UBA, Buenos Aires, Argentina
4Predictive Science, Inc., 9990 Mesa Rim Road, San Diego, CA 92121, USA
5Aryabhatta Research Institute of Observational Sciences (ARIES), Nainital, India - 263 129
6Naval Research Laboratory, Washington, DC, 20375, USA

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Abstract

We analyze the observations of two flares from NOAA AR 10501 on 20 November, 2003. The flares are homologous, exhibit four ribbons and are located in a quadrupolar magnetic configuration. The evolution of the ribbons suggests that the first eruption is triggered by “tether cutting” (with subsequent quadrupolar reconnection as in the “magnetic breakout” model), whereas the second one is consistent with the “magnetic breakout” model. Another interesting feature of our observations is the interaction of two filaments elongated in the north-south direction. The filaments merge at their central parts and afterwards change their orientation to the east-west direction. This merging and splitting is closely related to the evolution found in an MHD simulation as a result of reconnection between two flux ropes.

Fig. 1 Fig. 2
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Keywords : Sun: filaments – Sun: flares