Interplanetary phenomena associated with very intense geomagnetic storms |
| |
| Institution: | 1. Instituto Nacional Pesquisas Espaciais, 12201-970, São José dos Campos, São Paulo, Brazil;2. Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA;3. Goddard Space Flight Center, Greenbelt, MD, USA;4. Max Planck Institut fur Aeronomy, Lindau, Germany;1. Universidade do Vale do Paraíba /IP & D, São José dos Campos, SP, Brazil;2. Haystack Observatory, Massachusetts Institute of Technology (MIT), Westford, Massachusetts, USA;3. Department of Physics, University of Lagos, Akoka, Lagos, Nigeria;4. Instituto Nacional de Pesquisas Espaciais (INPE), São José dos Campos, SP, Brazil;5. Instituto Tecnológico de Aeronáutica (ITA), Divisão de Ciências Fundamentais, São José dos Campos, SP, Brazil;6. Facultad de Ciencias Astronómicas y Geofísicas, Universidad Nacional de La Plata, La Plata, Argentina;7. S.H College Thevara, Kochi-13, Mahatma Gandhi University, India;1. State Key Laboratory of Space Weather, National Space Science Center, Chinese Academy of Sciences, Beijing 100190, China;2. China-Brazil Joint Laboratory for Space Weather, Chinese Academy of Sciences, São Jose dos Campos, Brazil;3. School of Physics and Electronics Engineering, Hainan Normal University, Haikou 571158, China;1. Department of Electrical Engineering, Korea University, Seoul 136-713, Republic of Korea;2. Department of Electronic Materials Engineering, Kwangwoon University, Seoul 139-701, Republic of Korea;1. Environmental Physics Laboratory, Universidade de Vigo, Ourense 32004, Spain;2. Instituto de Geofìsica, Universidad Nacional Autonoma de Mexico, México D. F. 04510, Mexico;1. Department of Chemistry, The New College, Kolhapur, Maharashtra, 416012, India;2. Shivaji University, Kolhapur, Maharashtra, 416004, India |
| |
| Abstract: | The dominant interplanetary phenomena that are frequently associated with intense magnetic storms are the interplanetary manifestations of fast coronal mass ejections (CMEs). Two such interplanetary structures, involving an intense and long duration Bs component of the IMF are: the sheath region behind a fast forward interplanetary shock, and the CME ejecta itself. Frequently, these structures lead to the development of intense storms with two-step growth in their main phases.These structures, when combined, lead sometimes to the development of very intense storms, especially when an additional interplanetary shock is found in the sheath plasma of the primary structure accompanying another stream. The second stream can also compress the primary cloud, intensifying the Bs field, and bringing with it an additional Bs structure. Thus, at times very intense storms are associated with three or more Bs structures.Another aspect that can contribute to the development of very intense storms refers to the recent finding that magnetic clouds with very intense core magnetic fields tend to have large velocities, thus implying large amplitude interplanetary electric fields that can drive very intense magnetospheric energization. |
| |
| Keywords: | |
| 本文献已被 ScienceDirect 等数据库收录！ |
|
