Three-Dimensional Global Simulation of Coronal Mass Ejections with Flux-Rope Structures

Details Three-Dimensional Global Simulation of Coronal Mass Ejections with Flux-Rope Structures Three-Dimensional Global Simulation of Coronal Mass Ejections with Flux-Rope Structures

Dec 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010agufmsh32a..04w&link_type=abstract

American Geophysical Union, Fall Meeting 2010, abstract #SH32A-04

Physics

Plasma Physics

[2101] Interplanetary Physics / Coronal Mass Ejections, [2111] Interplanetary Physics / Ejecta, Driver Gases, And Magnetic Clouds, [7836] Space Plasma Physics / Mhd Waves And Instabilities, [7959] Space Weather / Models

Scientific paper

Three-dimensional (3-D), global, magnetohydrodynamic (MHD) models have been utilized in the past decade to study the initiation of CMEs and their evolution from the Sun to the Earth's environment and beyond. Most modelers used either plasma cloud, pressure or velocity pulses to investigate the structures of CMEs. The strength of the magnetic field from these computed results have always been lower than the in-situ measurements at 1 AU because the flux-rope structures were not included in these earlier models. In order to resolve this problem, we are developing a global 3-D, MHD simulation model which is capable of constructing the flux-rope structures. The new model consists of three physics based models: (1) a flux-rope MHD model (Wu et al., JGR, 104, 14789, 1999) is used to produce the CME structure, (2) the HAFv2 modified kinematic model (Fry et al., JGR, 106, 20985, 2001) is used to reproduce the back ground solar wind within 18 solar radii (Rs), and (3) a 3-D MHD model (Han et al, Comput. Fluids, 16, 81, 1988) is used to compute solar wind structure beyond 18 Rs. We will use the model to simulate a well-known CME event, which occurred on 12 May, 1997. Results will be compared with in-situ observations at 1 AU, and with previous non-flux-rope simulation results (e.g, Odstrcil et al., JGR, 109, A02116, 2004; Wu et al. JGR, 112, A09104, 2007).

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