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Center for Space Environment Modeling W. Manchester 1, I. Roussev, I.V. Sokolov 1, 1 University of Michigan AGU Berkeley March.

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Presentation on theme: "Center for Space Environment Modeling W. Manchester 1, I. Roussev, I.V. Sokolov 1, 1 University of Michigan AGU Berkeley March."— Presentation transcript:

1 Center for Space Environment Modeling http://csem.engin.umich.edu W. Manchester 1, I. Roussev, I.V. Sokolov 1, 1 University of Michigan AGU Berkeley March 1, 2003 Modeling the May 1, 1998 CME propagation

2 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) = n 0 + n 1 T/T 0 n 0 =4 n 1 = 9  Magnetic field specified by magnetogram data obtained by the Wilcox Solar Observatory

3 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).

4 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.

5 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).

6 Center for Space Environment Modeling http://csem.engin.umich.edu False color image of velocity magnitude with field lines shown in white

7 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

8 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

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