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)
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.
Fig. 2: Zoom view of the previous figure with the integration grid also shown.
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.
Fig. 4: Zoom view of the previous figure.
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.