Actors of the main activity in large complex centres during the 23 solar cycle maximum |
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| Authors: | B Schmieder P Démoulin E Pariat T Török G Molodij CH Mandrini S Dasso R Chandra W Uddin P Kumar PK Manoharan P Venkatakrishnan N Srivastava |
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| Institution: | 1. Observatoire de Paris, LESIA, 92195 Meudon, France;2. Instituto de Astronom?´a y F?´sica del Espacio (UBA-CONICET) and Facultad de Ciencias Exactas y Naturales (UBA), Buenos Aires, Argentina;3. Department of Physics, DSB Campus, Kumaun University, Nainital 263 002, Uttarakhand, India;4. ARIES, Manora Peak, Nainital 263 129, India;5. Radio Astronomy Centre, Tata Institute of Fundamental research, Udhagamandalam (Ooty) 643 001, India;6. Udaipur Solar Observatory, P.O. Box, 198, Dewali, Udaipur 313 001, India |
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| Abstract: | During the maximum of Solar Cycle 23, large active regions had a long life, spanning several solar rotations, and produced large numbers of X-class flares and CMEs, some of them associated to magnetic clouds (MCs). This is the case for the Halloween active regions in 2003. The most geoeffective MC of the cycle (Dst = −457) had its source during the disk passage of one of these active regions (NOAA 10501) on 18 November 2003. Such an activity was presumably due to continuous emerging magnetic flux that was observed during this passage. Moreover, the region exhibited a complex topology with multiple domains of different magnetic helicities. The complexity was observed to reach such unprecedented levels that a detailed multi-wavelength analysis is necessary to precisely identify the solar sources of CMEs and MCs. Magnetic clouds are identified using in situ measurements and interplanetary scintillation (IPS) data. Results from these two different sets of data are also compared. |
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| Keywords: | Active region Coronal mass ejection Magnetic clouds Magnetic helicity |
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