HR: 0800h
AN: SH31A-1178    [Abstracts]
TI: Orientation Of Interplanetary Magnetic Clouds Associated With Filament Eruptions And Major Geomagnetic Storms
AU: * Wang, Y
EM: ymwang@ustc.edu.cn
AF: School of Earth & Space Sci., Univ. of Sci. & Tech. of China, 96#, Jinzhai RD, Hefei, Anhui, 230026 China
AU: Ye, P
EM: pzye@ustc.edu.cn
AF: School of Earth & Space Sci., Univ. of Sci. & Tech. of China, 96#, Jinzhai RD, Hefei, Anhui, 230026 China
AU: Zhou, G
EM: zhougp@ourstar.bao.ac.cn
AF: National Astronomical Observatories of China, A20, Datun RD, Chaoyang Dist., Beijing, 100012 China
AU: Wang, S
EM: swan@ustc.edu.cn
AF: School of Earth & Space Sci., Univ. of Sci. & Tech. of China, 96#, Jinzhai RD, Hefei, Anhui, 230026 China
AU: Wang, J
EM: wjx@ourstar.bao.ac.cn
AF: National Astronomical Observatories of China, A20, Datun RD, Chaoyang Dist., Beijing, 100012 China
AB: As a major source of non-recurrent geomagnetic storms, more than half of magnetic clouds in the interplanetary medium are associated with filament eruptions [Subramanian and Dere, 2001]. The strength of south component of the magnetic field inside magnetic cloud and its duration are consider the very important factors in causing geomagnetic storm. Obviously, these factors are related to the orientation of magnetic cloud in terms of flux rope model. By investigating the observations of SOHO and ACE spacecraft from 2000 to 2003, the relationship between the orientation of interplanetary magnetic clouds which were associated with filament eruptions and major geomagnetic storms are studied. Two issues are discussed: (1) the effect of magnetic cloud's orientation on the intensity of geomagnetic storm, and (2) the possible factors in influencing the cloud's orientation. The results will be worked out.
UR: http://staff.ustc.edu.cn/~ymwang/mc_orientation.htm
DE: 7500 SOLAR PHYSICS, ASTROPHYSICS, AND ASTRONOMY
DE: 7513 Coronal mass ejections
DE: 7531 Prominence eruptions
DE: 2100 INTERPLANETARY PHYSICS
DE: 2111 Ejecta, driver gases, and magnetic clouds
SC: SPA-Solar and Heliospheric Physics [SH]
MN: 2004 AGU Fall Meeting