Center for Space Environment Modeling

http://csem.engin.umich.edu

W. Manchester1, I. Roussev, I.V. Sokolov1,

1University of Michigan

AGUBerkeley

March 1, 2003

Modeling the May 1, 1998 CME propagation

Center for Space Environment Modeling

http://csem.engin.umich.edu

Carrington Rotation 1935

The 3D model of Roussev, 2003 ApJ, volume 595, pages L57

Internal degrees of freedom depend on temperature (n+2)/n n(T) = n0 + n1T/T0 n0 =4 n1 = 9

Magnetic field specified by magnetogram data obtained by the Wilcox Solar Observatory

Center for Space Environment Modeling

http://csem.engin.umich.edu

The Ambient Solar Wind

Magnetic and velocity structure are shown for the steady-state solar wind solution. The purple sheet shows the current sheet while high speed wind is shown as orange (760 km/s) and slow speed wind as green (470 km/s).

Center for Space Environment Modeling

http://csem.engin.umich.edu

View of the wind at 1 AU

False color image shows the wind speed at 1 AU, while contour lines show the magnetic field strength.

Center for Space Environment Modeling

http://csem.engin.umich.edu

Properties of the Initial State

Magnetic field lines shown in white superimposed on false color images of density (left) and magnetic field strength (right).

Center for Space Environment Modeling

http://csem.engin.umich.edu

False color image of velocity magnitude with field lines shown in white

QuickTime™ and aBMP decompressorare needed to see this picture.

Center for Space Environment Modeling

http://csem.engin.umich.edu

3D View and view on the Equatorial Plane

False color images of velocity magnitude with white magnetic field lines at t = 0.53 hours

Center for Space Environment Modeling

http://csem.engin.umich.edu

Features of the Model

CME initiated by force imbalance Flux rope propagates from active region 8210 AMR essential to treat the many length scales of the system including active

region length scale in a 3D corona based on magnetic synoptic maps Future simulations will take the CME to 1 AU and use model output to drive

magnetospheric simulations