C. May 12, 1997 Interplanetary Event

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

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

CME Cone Model

Conceptual model:CME as a shell-like region

of enhanced densityGeometrical and kinematical fitting:

Dependence of predicted CME haloson the latitude, longitude, angular

width, and velocity[ Zhao et al., 2001 ]

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 Rs

(14:15 UT)• acceleration: 18.5 m/s2

Boundary Conditions

Ambient Solar WindAmbient Solar Wind

+ Plasma Cloud

CASE - 1 CASE - 2

Evolution of Parameters at Earth

Ambient Solar WindAmbient Solar Wind

+ Plasma Cloud

CASE - 1 CASE - 2

May 12, 1997 Interplanetary Event

ICME propagates into bi-modal solar wind

May 12, 1997 Interplanetary Event

Fast stream follows the ICME

May 12, 1997 Interplanetary Event

ICME propagates into enhanced density at CIR

May 12, 1997 Interplanetary Event

IMF is distorted by shock compression and draping around ICME

May 12, 1997 Interplanetary Event

May 12, 1997 Interplanetary Event

May 12, 1997 Interplanetary Event

May 12, 1997 Interplanetary Event