On the dynamics of the solar corona: the numerics behind a self-consistent 3D MHD model

Details On the dynamics of the solar corona: the numerics behind a self-consistent 3D MHD model On the dynamics of the solar corona: the numerics behind a self-consistent 3D MHD model

Dec 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002esasp.506...51k&link_type=abstract

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

Physics

Mhd, Solar Wind, Numerical Simulations

Scientific paper

Space missions like SOHO have renewed the interest in the physics of the solar corona. This complex system is not yet fully understood due to lack of sufficiently detailed observations, and also because realistic models should cover processes occurring on various spatial scales, while being both multidimensional and time-dependent. Significant progress w.r.t. their numerical realization was achieved recently with the Central Weighted Essentially Non-Oscillatory scheme. A 3rd order CWENO scheme efficiently capturing strong gradients forms the basis of our new code. After describing the algorithm and its implementation, we present test results as well as comparisons with preexisting codes.

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