Cosmic Structure Formation and Dynamics: Magnetohydrodynamic Simulations of Coronal Heating

Abstract

By implementing a three-dimensional magnetohydrodynamic (MHD) code based on the CIP-MOCCT scheme, we carried out large scale MHD simulations of the solar atmosphere covering the region from the convection zone to the corona. We found that in regions with weak magnetic fields (B~100G), horizontal magnetic loops created in the upflow regions of the convection generate high frequency waves by reconnecting with the ambient magnetic fields. The corona can be heated up by direct heating by magnetic reconnection and dissipation of high frequency waves generated by the magnetic reconnection.

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Cite this paper

@inproceedings{Matsumoto2009CosmicSF, title={Cosmic Structure Formation and Dynamics: Magnetohydrodynamic Simulations of Coronal Heating}, author={Ryoji Matsumoto and H. Isobe}, year={2009} }