HR: 1330h
AN: SH43A-02    [Abstracts]
TI: The Global Magnetic Topology of the Solar Corona Preceding CME Eruptions
AU: * Ledvina, S A
EM: ledvina@ssl.berkeley.edu
AF: Space Sciences Lab, UC Berkeley, 7 Gauss Way # 7450, Berkeley, CA 94720-7450 United States
AU: Luhmann, J G
EM: jgluhman@ssl.berkeley.edu
AF: Space Sciences Lab, UC Berkeley, 7 Gauss Way # 7450, Berkeley, CA 94720-7450 United States
AU: Li, Y
EM: yanli@ssl.berkeley.edu
AF: Space Sciences Lab, UC Berkeley, 7 Gauss Way # 7450, Berkeley, CA 94720-7450 United States
AU: Abbett, B
EM: abbett@ssl.berkeley.edu
AF: Space Sciences Lab, UC Berkeley, 7 Gauss Way # 7450, Berkeley, CA 94720-7450 United States
AU: Arge, C
EM: Nick.Arge@hanscom.af.mil
AF: AFRL/VSBXS, 29 Randolph Rd., Hanscom AFB, MA 01731-3010 United States
AB: Understanding coronal mass ejections (CMEs) is a key step to understanding and eventually predicting Space Weather. Three CME event periods have gained great interest lately due to the wide range of observations made before, during and after each event. These include the Halloween storms from October 2003, the eruption involving AR 8210 during CR 1935, and the May 12, 1997 halo CME. These events have been selected by several groups as an example of a real event that they will try to simulate. We present preliminary results of MHD simulations of the pre-eruption global coronal magnetic topology for each event, using a synoptic map-based ZEUS-3D MHD model of the solar corona. We compare and contrast the results to gain insight into the prevailing conditions, especially the open/closed field configurations surrounding the event sites.
DE: 7509 Corona
DE: 7511 Coronal holes
DE: 7524 Magnetic fields
SC: SPA-Solar and Heliospheric Physics [SH]
MN: 2005 Joint Assembly