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Modeling the May 1, 1998 CME propagation

Modeling the May 1, 1998 CME propagation. W. Manchester 1 , I. Roussev, I.V. Sokolov 1 , 1 University of Michigan AGU Berkeley March 1, 2003. Carrington Rotation 1935. The 3D model of Roussev, 2003 ApJ, volume 595, pages L57

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Modeling the May 1, 1998 CME propagation

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  1. Modeling the May 1, 1998 CME propagation W. Manchester1, I. Roussev, I.V. Sokolov1, 1University of Michigan AGU Berkeley March 1, 2003

  2. Carrington Rotation 1935 • The 3D model of Roussev, 2003 ApJ, volume 595, pages L57 • Internal degrees of freedom depend on temperature g = (n+2)/n n(T) = n0 + n1T/T0 n0 =4 n1 = 9 • Magnetic field specified by magnetogram data obtained by the Wilcox Solar Observatory

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

  7. 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. 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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