AAS 204th Meeting, June 2004
Session 67 Solar Input to the Heliosphere
SPD Topical Session, Wednesday, June 2, 2004, 2:30-4:00pm, 4:15-6:00pm, 704/706

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[67.09] CMEs and CME Shock Evolution on Different Background Winds

B. Van der Holst, S. Poedts, C. Jacobs, E. Chane, I. Chattopadhyay, D. Shapakidze, D. Banerjee (CPA)

Coronal Mass Ejections (CMEs) play a key role in many Space Weather phenomena and are important for prediction models as well. A short overview is given of the different types of CME models and different triggering mechanisms currently under study. The shocks in the solar corona and interplanetary (IP) space caused by fast Coronal Mass Ejections (CMEs) are simulated numerically and their complex structure and evolution is studied in the framework of magnetohydrodynamics (MHD). The complexity of these shocks is caused by the presence of three characteristic velocities and the anisotropy induced by the magnetic field. As a result, the CME shocks generated in the lower corona can have a complex topology including secondary shock fronts, over-compressive and compound shocks, etc. The evolution of these CME shocks is followed during their propagation through the solar wind and, in particular, though the critical points in the wind. Particular attention is given to the effect of the background wind. Different, `frequently used' wind models are reconstructed with the same numerical code and the same resolution. Also different, 'popular' CME models are reconstructed. Then, the different CME models are combined with the different wind models. The results are sometimes surprising.

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