Shell-Model Simulations of MHD in a Solar Coronal Loop

Details Shell-Model Simulations of MHD in a Solar Coronal Loop Shell-Model Simulations of MHD in a Solar Coronal Loop

May 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005agusmsp14a..05b&link_type=abstract

American Geophysical Union, Spring Meeting 2005, abstract #SP14A-05

Statistics

7509 Corona, 7519 Flares, 7524 Magnetic Fields, 7853 Spacecraft/Atmosphere Interactions, 7863 Turbulence

Scientific paper

Statistics may be necessary to keep a global view of the complexity of astrophysical turbulence, in particular the effects of non-linear interactions over a wide range of scales. However, from the numerical point of view, a statistical approach to turbulence has the contradictory needs for computing speed and for a good description of the solutions of the MHD equations. This problem can be addressed by simplified models like cellular automata or shell-models. In the shell-models, the low number of well-chosen modes allows to keep the most possible of the complex and non-linear physics of the MHD equations while running sufficiently fast to produce statistics of fields, of structures, and of "events". The model we present here is designed to represent a magnetic loop in the solar corona. It consists of a pile of shell-models, which allows to reach a wide range of wavenumbers in cross-sections of the loop and model the non-linear couplings between these modes. The shell-models are also coupled by Alfvén waves propagating along the loop. We study the statistical properties of intermittent energy dissipation and of the velocity and magnetic fields produced by this model. These statistical properties can be compared to statistics issued from observations, like structure functions or events distributions.

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