HR: 0800h
AN: SH51C-1230    [Abstracts]
TI: Characteristics of the Interplanetary Coronal Mass Ejections in the Heliosphere Between 0.3 and 5.4 AU
AU: * Wang, C
EM: cw@spaceweather.ac.cn
AF: Key Laboratory of Space Weather, Chinese Academy of Sciences, P.O.Box 8701, Beijing, 100080 China
AU: Du, D
EM: ddu@spaceweather.ac.cn
AF: Key Laboratory of Space Weather, Chinese Academy of Sciences, P.O.Box 8701, Beijing, 100080 China
AU: Richardson, J D
EM: jdr@space.mit.edu
AF: Kavli Institute for Astrophysics and Space Research, Massachussetts Institute of Technology, 77 Mass. Ave., Cambridge, MA 02139 United States
AB: We identify and characterize interplanetary coronal mass ejections (ICMEs) observed by spacecraft in the solar wind, namely Helios 1 and 2, PVO, ACE and Ulysses, which together cover heliocentric distances from 0.3 to 5.4 AU. The primary identification signature used to look for ICMEs is abnormally low proton temperatures. About 600 probable ICMEs were identified from the solar wind plasma and magnetic field data from these spacecraft. We use these events to study the radial evolution of ICMEs between 0.3 and 5.4 AU, mainly in a statistical sense. The occurrence rate of ICME approximately follows the solar activity cycle. ICMEs expand as they move outward since the internal pressure is generally larger than the external pressure. The average radial width of ICMEs increases with distance. ICMEs expand by a factor of 2.7 in radial width between 1 and 5 AU. The radial expansion speed of ICMEs decreases with distance and is of the order of the Alfven speed. The density and magnetic field magnitude decrease faster in ICMEs, which fall off with distance R as R^-2.4 and R^-1.5, respectively, than in the ambient solar wind; However the temperature decreases as R^-0.7, slightly less rapid than in the ambient solar wind. These results are consistent with previous findings with relatively limited data coverage. We also use a one-dimensional MHD model to investigate the radial expansion of the ICMEs and find that the radial expansion speed is of the order of the Alfven speed, consistent with the observations.
DE: 2101 Coronal mass ejections (7513)
DE: 2111 Ejecta, driver gases, and magnetic clouds
DE: 2162 Solar cycle variations (7536)
SC: SPA-Solar and Heliospheric Physics [SH]
MN: Fall Meeting 2005