Numerical MHD Simulation of Flux-Rope Formed Ejecta Interaction with Bi-modal Solar Wind

Details Numerical MHD Simulation of Flux-Rope Formed Ejecta Interaction with Bi-modal Solar Wind Numerical MHD Simulation of Flux-Rope Formed Ejecta Interaction with Bi-modal Solar Wind

Dec 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001agufmsh11d..07w&link_type=abstract

American Geophysical Union, Fall Meeting 2001, abstract #SH11D-07

Physics

2164 Solar Wind Plasma, 7509 Corona, 7513 Coronal Mass Ejections, 7531 Prominence Eruptions

Scientific paper

Recent SOHO and WIND observations have shown that CMEs could be accelerated or decelerated due to their interactions with the solar wind. These interactions will result in different solar wind signatures. In order to understand the physics of CME interaction with non-uniform solar wind during propagation, we combined our previously developed two-dimensional planar bi-modal solar wind model (Wang et al. 1996) and streamer and flux-rope model (Wu et al. 1995) to study the fast and slow wind interactions with the propagating CME. This simulation is carried out up to the inner heliosphere ( ~30 Rs (solar radii)). The results will show the effect of CME propagation speed by the fast and slow speed solar wind, and the shock formation and their comparison with the uniform solar wind. Also the features of the deflection of CME propagation due to streamer will be discussed. STW and AHW acknowledge AFOSR, NSF, JPL, and AAMU subcontract of NASA prime contract. Wang, A. H., S. T. Wu, S. T. Suess, and G. Poletto, Global Model of Corona with Heat and Momentum Addition, J. Geophys. Res., 103, A2, 1413-1922, 1996. Wu, S. T., W. P. Guo, and J. F. Wang, Dynamical Evolution of Coronal Streamer Bubble System: I. A Self-consistent Planar Magnetohydrodynamic Simulation, Solar Physics, 157, 325-348, 1995.

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