Earth Planets Space, Vol. 61 (No. 5), pp. 599-602, 2009LETTER
Stefaan Poedts, Carla Jacobs, Bart van der Holst, Emmanuel Chané, and Rony Keppens
Centrum voor Plasma-Astrofysica, Katholieke Universiteit Leuven, Belgium
(Received October 31, 2007; Revised January 30, 2008; Accepted August 24, 2008; Online published May 29, 2009)
Numerical simulations of Coronal Mass Ejections (CMEs) can provide a deeper insight in the structure and propagation of these impressive solar events. In this work, we present our latest results of numerical simulations of the initial evolution of a fast CME. For this purpose, the equations of ideal MagnetoHydroDynamics (MHD) have been solved on a three-dimensional (3D) mesh by means of an explicit, finite volume solver, where the simulation domain ranges from the lower solar corona up to 30R. In order to simulate the propagation of a CME throughout the heliosphere, a magnetic flux rope is superposed on top of a stationary background solar (MHD) wind with extra density added to the flux rope. The flux rope is launched by giving it an extra initial velocity in order to get a fast CME forming a 3D shock wave. The magnetic field inside the initial flux rope is described in terms of Bessel functions and possesses a high amount of twist.
Key words: Magnetohydrodynamics, numerical, coronal mass ejections.