AAS 200th meeting, Albuquerque, NM, June 2002
Session 36. The Magnetic Structure of CMEs
Display, Tuesday, June 4, 2002, 10:00am-6:30pm, SW Exhibit Hall

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[36.02] Effects of Topology on CME Kinematic Properties

W. Liu, X. P. Zhao (W. W. Hansen Experimental Physics Laboratory, Stanford University), S. T. Wu (Center for Space Plasma and Aeronomic Research, The University of Alabama in Huntsville), P. H. Scherrer (W. W. Hansen Experimental Physics Laboratory, Stanford University)

Coronal Mass Ejections (CMEs) exhibit two types of kinematic property: fast CMEs with high initial speeds and slow CMEs with low initial speeds but gradual accelerations. Efforts have been made for years to probe the underlying physics responsible for this dual character. Within these efforts, magnetic topology has gained much attention. Low and Zhang (ApJ, 564, L53, 2002) proposed that fast or slow CMEs result from initial states with magnetic configurations characterized by the normal or inverse quiescent prominences, respectively. To test their theory and further explore the effects of topology on kinematic properties of CMEs, we employed a 2-D, axisymmetric, resistive MHD model to simulate the evolution of CMEs in the normal and inverse prominence environments, respectively. The numerical results show that the CMEs originating from a normal prominence environment do have higher initial speeds than those from an inverse one. In addition, our simulations demonstrate the distinct roles played by magnetic reconnection in these two topologically different magnetic environments to produce the two different CME height-time profiles as suggested by Low and Zhang. The implication of the results and discussion on future work are described. SOHO is a project of international cooperation between ESA and NASA.

If you would like more information about this abstract, please follow the link to http://sun.stanford.edu/~weiliu/muri/job1/topology-effects.html. This link was provided by the author. When you follow it, you will leave the Web site for this meeting; to return, you should use the Back comand on your browser.

The author(s) of this abstract have provided an email address for comments about the abstract: weiliu@sun.stanford.edu

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Bulletin of the American Astronomical Society, 34
© 2002. The American Astronomical Soceity.