ANGEO Annales Geophysicae ANGEO Ann. Geophys. 1432-0576 Copernicus Publications Göttingen, Germany 10.5194/angeo-27-989-2009 A novel code for numerical 3-D MHD studies of CME expansion Kleimann J. 1 Kopp A. 2 3 Fichtner H. 3 Grauer R. 4 Nordlys Observatoriet, Universitetet i Tromsø, 9037 Tromsø, Norway Institut für Experimentelle und Angewandte Physik, Christian-Albrechts-Universität zu Kiel, 24118 Kiel, Germany Institut für Theoretische Physik IV, Ruhr-Universität Bochum, 44780 Bochum, Germany Institut für Theoretische Physik I, Ruhr-Universität Bochum, 44780 Bochum, Germany 02 03 2009 27 3 989 1004 Copyright: © 2009 J. Kleimann et al. 2009 This work is licensed under the Creative Commons Attribution 3.0 Unported License. To view a copy of this licence, visit https://creativecommons.org/licenses/by/3.0/ This article is available from https://angeo.copernicus.org/articles/27/989/2009/angeo-27-989-2009.html The full text article is available as a PDF file from https://angeo.copernicus.org/articles/27/989/2009/angeo-27-989-2009.pdf

A recent third-order, essentially non-oscillatory central scheme to advance the equations of single-fluid magnetohydrodynamics (MHD) in time has been implemented into a new numerical code. This code operates on a 3-D Cartesian, non-staggered grid, and is able to handle shock-like gradients without producing spurious oscillations. <br><br> To demonstrate the suitability of our code for the simulation of coronal mass ejections (CMEs) and similar heliospheric transients, we present selected results from test cases and perform studies of the solar wind expansion during phases of minimum solar activity. We can demonstrate convergence of the system into a stable Parker-like steady state for both hydrodynamic and MHD winds. The model is subsequently applied to expansion studies of CME-like plasma bubbles, and their evolution is monitored until a stationary state similar to the initial one is achieved. In spite of the model's (current) simplicity, we can confirm the CME's nearly self-similar evolution close to the Sun, thus highlighting the importance of detailed modelling especially at small heliospheric radii. <br><br> Additionally, alternative methods to implement boundary conditions at the coronal base, as well as strategies to ensure a solenoidal magnetic field, are discussed and evaluated.

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