MHD SIMULATIONS OF INTERPLANETARY CME-DRIVEN SHOCKS  

 

(FROM THE SUN TO EARTH'S ORBIT)  

 

R. Rodriguez-Gasen*, C.Jacobs**, A.Aran*, S.Poedts**   and B. Sanahuja*

* Departament d'Astronomia i Meteorologia. Universitat de Barcelona. Spain

** Centre for Plasma Astrophysics. Katholieke Universiteit Leuven. Belgium

Project sponsored by the Spanish DGCYT (MCyT) and DURSI (Generalitat de Catalunya)


 

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Fig. 1: General view of a snapshot of a three-dimensional simulation of the CME-driven shock in the 30 solar radii scenario. In grey the isosurface where the value of rhorel= 0.1. In the XY plane, contours of the rhorel (relative density with respect to the background solar wind density). The snapshot is taken after t=7.26 h.

 

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Fig. 2: Zoom view of the previous figure with the integration grid also shown.

 

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Fig. 3: General view of a snapshot of a three-dimensional simulation of the CME-driven shock in the 1AU scenario (Earth's orbit). In grey the isosurface where the value of rhorel= 0.1. In the YZ plane, contours of the solar wind radial velocity. The snapshot is taken after t=3.99 h.

 

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Fig. 4: Zoom view of the previous figure.

 

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Fig. 5: General view of a snapshot of a three-dimensional simulation of the CME-driven shock in the 1AU scenario (Earth's orbit). In grey the isosurface where the value of rhorel= 0.1. In the XZ plane, contours of the solar wind radial velocity. The snapshot is taken after t=19.81 h.

 

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