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Solar activity due to magnetic complexity of active regions

Published online by Cambridge University Press:  26 August 2011

Brigitte Schmieder ,
Cristina Mandrini ,
Ramesh Chandra ,
Pascal Démoulin ,
Tibor Török ,
Etienne Pariat  and
Wahab Uddin
Brigitte Schmieder
Affiliation:
Observatoire de Paris, LESIA, Meudon, 92195, France email: brigitte.schmieder@obspm.fr
Cristina Mandrini
Affiliation:
IAFE, CONICET-UBA (FCEN), Buenos Aires, Argentina email: mandrini@iafe.uba.ar
Ramesh Chandra
Affiliation:
Observatoire de Paris, LESIA, Meudon, 92195, France email: brigitte.schmieder@obspm.fr
Pascal Démoulin
Affiliation:
Observatoire de Paris, LESIA, Meudon, 92195, France email: brigitte.schmieder@obspm.fr
Tibor Török
Affiliation:
Observatoire de Paris, LESIA, Meudon, 92195, France email: brigitte.schmieder@obspm.fr
Etienne Pariat
Affiliation:
Observatoire de Paris, LESIA, Meudon, 92195, France email: brigitte.schmieder@obspm.fr
Wahab Uddin
Affiliation:
ARIES, Nainital, India
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Abstract

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Active regions (ARs), involved in the Halloween events during October-November 2003, were the source of unusual activity during the following solar rotation. The flares on 18-20 November 2003 that occur in the AR NOAA10501 were accompanied by coronal mass ejections associated to some particularly geoeffective magnetic clouds.

Our analysis of the magnetic flux and helicity injection revealed that a new emerging bipole and consequent shearing motions continuously energized the region during its disk passage. The stored energy was eventually released through the interaction of the various systems of magnetic loops by several magnetic reconnection events. Active events on November 18 (filament eruptions and CMEs) were originated by shearing motions along a section of the filament channel that injected magnetic helicity with sign opposite to that of the AR. Two homologous flares, that occurred on November 20, were apparently triggered by different mechanisms as inferred from the flare ribbons evolution (filament eruption and CMEs). We studied in detail the behaviour of two North-South oriented filaments on November 20 2003. They merged and split following a process suggestive of ‘sling-shot’ reconnection between two coronal flux ropes. We successfully tested this scenario in a 3D MHD simulation that is presented in this paper.

Keywords

Active regionmagnetic helicityfilament reconnection
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 6 , Symposium S273: The Physics of Sun and Star Spots , August 2010 , pp. 164 - 168
Copyright
Copyright © International Astronomical Union 2011

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