1. C. May 12, 1997 Interplanetary Event

2. May 12, 1997 Interplanetary Coronal Mass Ejection Event CU/CIRES, NOAA/SEC, SAIC, Stanford Tatranska Lomnica, Slovakia, June 23-28, 2003 D. Odstrcil, P. Riley, C. N. Arge, X. P Zhao, and V. J. Pizzo

3. Ambient Solar Wind Models SAIC 3-D MHD steady state coronal model based on photospheric field maps CU/CIRES-NOAA/SEC 3-D solar wind model based on potential and current-sheet source surface empirical models

4. CME Cone Model Conceptual model: CME as a shell-like region of enhanced density Geometrical and kinematical fitting: Dependence of predicted CME halos on the latitude, longitude, angular width, and velocity [ Zhao et al., 2001 ]

5. CME Cone Model [ Zhao et al., 2001 ] Best fitting for May 12, 1997 halo CME latitude: N3.0 longitude: W1.0 angular width: 50 deg velocity:650 km/s at 24 R s (14:15 UT) acceleration: 18.5 m/s 2

6. Boundary Conditions Ambient Solar Wind + Plasma Cloud CASE - 1 CASE - 2

7. Evolution of Parameters at Earth Ambient Solar Wind + Plasma Cloud CASE - 1 CASE - 2

8. May 12, 1997 Interplanetary Event ICME propagates into bi-modal solar wind

9. May 12, 1997 Interplanetary Event Fast stream follows the ICME

10. May 12, 1997 Interplanetary Event ICME propagates into enhanced density at CIR

11. May 12, 1997 Interplanetary Event IMF is distorted by shock compression and draping around ICME

12. May 12, 1997 Interplanetary Event