On the dynamics of the solar corona: first results obtained with a new 3D MHD model

Details On the dynamics of the solar corona: first results obtained with a new 3D MHD model On the dynamics of the solar corona: first results obtained with a new 3D MHD model

Dec 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002esasp.506...21k&link_type=abstract

In: Solar variability: from core to outer frontiers. The 10th European Solar Physics Meeting, 9 - 14 September 2002, Prague, Cze

Physics

Solar Wind, Mhd, Numerical Simulation, Two-Fluid Modeling, Cweno

Scientific paper

A newly developed self-consistent 3D MHD code (see poster by Kleimann et al., this conference) is applied to the problem of the dynamcis of the solar corona. First, we present the basic system of equations for a two-fluid description of the solar wind plasma and point out possible numerical difficulties arising from an improper choice of variables. Second, we perform a study of the solar wind expansion during phases of minimum solar activity, serving mainly as a first "real world" test case. Third, we discuss first results of the application of the model to propagating disturbances, such as coronal mass ejections and/or shocks.

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