Studying the Complexity in Dynamics and Magnetic Topology of CME with 3D MHD Simulations Involving Dynamic AMR

Details Studying the Complexity in Dynamics and Magnetic Topology of CME with 3D MHD Simulations Involving Dynamic AMR Studying the Complexity in Dynamics and Magnetic Topology of CME with 3D MHD Simulations Involving Dynamic AMR

Publishing date

May 2002

URL

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002agusmsh21a..01r&link_type=abstract

Journals

American Geophysical Union, Spring Meeting 2002, abstract #SH21A-01

Science

Statistics

Field

Computation

Additional info 3

7509 Corona, 7513 Coronal Mass Ejections, 7843 Numerical Simulation Studies, 2111 Ejecta, Driver Gases, And Magnetic Clouds

Type

Scientific paper

Abstract

It is of fundamental importance in solar, heliospheric, and magnetospheric physics to explore the high degree of variability and complex internal magnetic and plasma structure of CMEs. Three-dimensional (3D) magnetohydrodynamic (MHD) simulations provide excellent grounds for studying the complexity in dynamics of this and other solar phenomena. We present some results on state-of-art numerical experiments of CME propagation, including dynamic Adaptive Mesh Refinement (AMR). All computations presented here are carried out using the BATS-R-US (Block Adaptive Tree Solarwind Roe Upwind Scheme) code and involve 3D MHD. The CME is initiated through an eruption of twisted flux rope in the solar corona. The MHD shock created ahead of the CME is essential in determining geoeffective events. The physics based AMR allows to reveal the complexity of the CME development and propagation on the particular ray Sun-Earth. The applied numerical algorithm is designed to use optimal computational resources for the sake of tracing CMEs with very high spatial resolution all the way from Sun to Earth, and beyond. We further discuss the differences in using various criteria for mesh refinement on the overall physical picture of the CME dynamics.

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