HR: 0800h
AN: SH32A-0785    [Abstracts]
TI: Modeling STEREO White-Light Observations of CMEs with 3D MHD Simulations
AU: * Manchester, M B
EM: chipm@umich.edu
AF: University of Michigan, 2455 Hayward Street, Ann Arbor, MI 48109, United States
AU: Vourlidas, A
EM: avourlid@nrl.navy.mil
AF: Naval Research Laboratory, Overlook Ave SW, Washington, DC 20375, United States
AU: Toth, G
EM: gtoth@grid.engin.umich.edu
AF: University of Michigan, 2455 Hayward Street, Ann Arbor, MI 48109, United States
AU: Lugaz, N
EM: nlugaz@ifa.hawaii.edu
AF: Institute for Astronomy, University of Hawaii, Honolulu, HI 96822,
AU: Sokolov, I
EM: igorsok@umich.edu
AF: University of Michigan, 2455 Hayward Street, Ann Arbor, MI 48109, United States
AU: Gombosi, T
EM: tamas@umich.edu
AF: University of Michigan, 2455 Hayward Street, Ann Arbor, MI 48109, United States
AU: De Zeeuw, D
EM: darrens@umich.edu
AF: University of Michigan, 2455 Hayward Street, Ann Arbor, MI 48109, United States
AU: Opher, M
EM: mopher@gmu.edu
AF: George Mason University4400 University Drive, 4400 University Drive, Fairfax, VA 22030, United States
AB: We model the Thomson-scattered white-light appearance of a variety of 3D MHD models of CMEs during solar minimum to reproduce large-scale features of SECCHI observations. We create a gallery of expected CME shapes at large elongations as seen by SECCHI. We examine evidence of shock propagation, magnetic clouds, CME pancaking, and complex time evolution as CMEs propagate at large elongation past the Thomson sphere. A key point is to determine how the structure of CMEs and CME-driven shocks are affected by interaction with the ambient solar wind. MHD models are performed with BATSRUS and SWMF, and formulated by first arriving at a steady state corona and solar wind employing synoptic magnetograms. We initiate CMEs from active regions low in the corona with magnetic flux ropes.
DE: 7509 Corona
DE: 7513 Coronal mass ejections (2101)
DE: 7514 Energetic particles (2114)
DE: 7531 Prominence eruptions
DE: 7984 Space radiation environment
SC: SPA-Solar and Heliospheric Physics [SH]
MN: 2007 Fall Meeting