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R.W. Walsh, K. Galsgaard (U of StA)
The three-dimensional nature of the coronal magnetic field is very important in understanding the complex structures that we observe. Recent high cadence observations of the photospheric magnetic field reveal a continually changing environment where the magnetic field fragments are in continual motion relative to one another. This motion of what has been termed the Sun's Magnetic Carpet could be a possible source of the large amount of energy that is heating the quiet corona.
A three-dimensional MHD resistive numerical code is introduced to model the above dynamic scenerio. The situation is idealised by considering the case of two unbalanced magnetic patches that are rotated relative to one other. Results for the evolving magnetic structure, simplified plasma response and calculated total energy release will be presented. Implications of these results upon solar observations will be discussed.
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The author(s) of this abstract have provided an email address for comments about the abstract: robert@mcs.st-and.ac.uk