Abstract
Abstract 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 e. 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.
Highlights
It is generally accepted that coronal mass ejections (CMEs) originate from the so-called ‘closed’ magnetic regions on the Sun, consisting of thousands of magnetic loops
Since in the applied background coronal model for solar minimum the only polarity inversion line coincides with the equator, the flux rope solution is placed above the solar equator in the present simulation
The initially highly twisted magnetic field in the flux rope reconnects with the overlying magnetic field, but the magnetic field lines in the Coronal Mass Ejections (CMEs) remain connected to the solar surface
Summary
It is generally accepted that coronal mass ejections (CMEs) originate from the so-called ‘closed’ magnetic regions on the Sun, consisting of thousands of magnetic loops. (2006) demonstrated that 2.5D simulations with a simple CME model, consisting of a high-density plasma blob including a magnetic flux rope, can predict the flow variables at 1 AU for a specific CME event reasonably well. (2006), but in stead of launching a spherical plasma blob, a more advanced magnetic flux rope model, with an enhanced density, is flung into the interplanetary medium by giving it an initial velocity profile.
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