Actors of the main activity in large complex centres during the 23 solar cycle maximum
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 o...
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todo:paper_02731177_v47_n12_p2081_Schmieder2023-10-03T15:15:41Z Actors of the main activity in large complex centres during the 23 solar cycle maximum Schmieder, B. Démoulin, P. Pariat, E. Török, T. Molodij, G. Mandrini, C.H. Dasso, S. Chandra, R. Uddin, W. Kumar, P. Manoharan, P.K. Venkatakrishnan, P. Srivastava, N. Active region Coronal mass ejection Magnetic clouds Magnetic helicity Active regions Complex topology Coronal mass ejection Helicities In-situ measurement Interplanetary scintillation Long life Magnetic clouds Magnetic helicity Multiple domains Multiwavelength Solar cycle Solar rotation Solar source X-class flares Clouds Extraterrestrial atmospheres Magnetic flux Solar energy Solar system Magnetic domains 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. © 2010 Published by Elsevier Ltd. on behalf of COSPAR. Fil:Mandrini, C.H. Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales; Argentina. Fil:Dasso, S. Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales; Argentina. JOUR info:eu-repo/semantics/openAccess http://creativecommons.org/licenses/by/2.5/ar http://hdl.handle.net/20.500.12110/paper_02731177_v47_n12_p2081_Schmieder |
| institution |
Universidad de Buenos Aires |
| institution_str |
I-28 |
| repository_str |
R-134 |
| collection |
Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA) |
| topic |
Active region Coronal mass ejection Magnetic clouds Magnetic helicity Active regions Complex topology Coronal mass ejection Helicities In-situ measurement Interplanetary scintillation Long life Magnetic clouds Magnetic helicity Multiple domains Multiwavelength Solar cycle Solar rotation Solar source X-class flares Clouds Extraterrestrial atmospheres Magnetic flux Solar energy Solar system Magnetic domains |
| spellingShingle |
Active region Coronal mass ejection Magnetic clouds Magnetic helicity Active regions Complex topology Coronal mass ejection Helicities In-situ measurement Interplanetary scintillation Long life Magnetic clouds Magnetic helicity Multiple domains Multiwavelength Solar cycle Solar rotation Solar source X-class flares Clouds Extraterrestrial atmospheres Magnetic flux Solar energy Solar system Magnetic domains Schmieder, B. Démoulin, P. Pariat, E. Török, T. Molodij, G. Mandrini, C.H. Dasso, S. Chandra, R. Uddin, W. Kumar, P. Manoharan, P.K. Venkatakrishnan, P. Srivastava, N. Actors of the main activity in large complex centres during the 23 solar cycle maximum |
| topic_facet |
Active region Coronal mass ejection Magnetic clouds Magnetic helicity Active regions Complex topology Coronal mass ejection Helicities In-situ measurement Interplanetary scintillation Long life Magnetic clouds Magnetic helicity Multiple domains Multiwavelength Solar cycle Solar rotation Solar source X-class flares Clouds Extraterrestrial atmospheres Magnetic flux Solar energy Solar system Magnetic domains |
| description |
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. © 2010 Published by Elsevier Ltd. on behalf of COSPAR. |
| format |
JOUR |
| author |
Schmieder, B. Démoulin, P. Pariat, E. Török, T. Molodij, G. Mandrini, C.H. Dasso, S. Chandra, R. Uddin, W. Kumar, P. Manoharan, P.K. Venkatakrishnan, P. Srivastava, N. |
| author_facet |
Schmieder, B. Démoulin, P. Pariat, E. Török, T. Molodij, G. Mandrini, C.H. Dasso, S. Chandra, R. Uddin, W. Kumar, P. Manoharan, P.K. Venkatakrishnan, P. Srivastava, N. |
| author_sort |
Schmieder, B. |
| title |
Actors of the main activity in large complex centres during the 23 solar cycle maximum |
| title_short |
Actors of the main activity in large complex centres during the 23 solar cycle maximum |
| title_full |
Actors of the main activity in large complex centres during the 23 solar cycle maximum |
| title_fullStr |
Actors of the main activity in large complex centres during the 23 solar cycle maximum |
| title_full_unstemmed |
Actors of the main activity in large complex centres during the 23 solar cycle maximum |
| title_sort |
actors of the main activity in large complex centres during the 23 solar cycle maximum |
| url |
http://hdl.handle.net/20.500.12110/paper_02731177_v47_n12_p2081_Schmieder |
| work_keys_str_mv |
AT schmiederb actorsofthemainactivityinlargecomplexcentresduringthe23solarcyclemaximum AT demoulinp actorsofthemainactivityinlargecomplexcentresduringthe23solarcyclemaximum AT pariate actorsofthemainactivityinlargecomplexcentresduringthe23solarcyclemaximum AT torokt actorsofthemainactivityinlargecomplexcentresduringthe23solarcyclemaximum AT molodijg actorsofthemainactivityinlargecomplexcentresduringthe23solarcyclemaximum AT mandrinich actorsofthemainactivityinlargecomplexcentresduringthe23solarcyclemaximum AT dassos actorsofthemainactivityinlargecomplexcentresduringthe23solarcyclemaximum AT chandrar actorsofthemainactivityinlargecomplexcentresduringthe23solarcyclemaximum AT uddinw actorsofthemainactivityinlargecomplexcentresduringthe23solarcyclemaximum AT kumarp actorsofthemainactivityinlargecomplexcentresduringthe23solarcyclemaximum AT manoharanpk actorsofthemainactivityinlargecomplexcentresduringthe23solarcyclemaximum AT venkatakrishnanp actorsofthemainactivityinlargecomplexcentresduringthe23solarcyclemaximum AT srivastavan actorsofthemainactivityinlargecomplexcentresduringthe23solarcyclemaximum |
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1807317910635413504 |