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3D Numerical Simulations of Coronal Tectonics

Published online by Cambridge University Press:  01 November 2006

I. De Moortel  and
K. Galsgaard
I. De Moortel
Affiliation:
School of Mathematics and Statistics, University of St Andrews, North Haugh, St Andrews, Fife KY16 9SS, Scotland email: ineke@mcs.st-and.ac.uk
K. Galsgaard
Affiliation:
Niels Bohr Institute, Julie Maries vej 30, 2100 Copenhagen Ø, Denmark email: kg@astro.ku.dk
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Abstract

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We present the results of numerical simulations of 3D magnetic reconnection driven by photospheric footpoint motions. The model consists of two positive and two negative sources, which are placed on opposite boundaries of the cubic domain. Two different types of photospheric motions are then considered, namely rotating and twisting of the sources. These different footpoint motions result in a difference in the evolution of the magnetic skeleton and the location and efficiency of the energy build up. Both the dynamical evolution and the corresponding potential evolution of each system is investigated and a comparison is made between the energy storage and release that occurs at separators and separatrix surfaces.

Keywords

Sun: coronamagnetic fieldsactivity
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 2 , Symposium S233: Solar Activity and its Magnetic Origin , March 2006 , pp. 149 - 156
Copyright
© 2006 International Astronomical Union