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Simulations of shock structures of a flare/CME event in the low corona

Published online by Cambridge University Press:  01 September 2008

Jens Pomoell ,
Rami Vainio  and
Silja Pohjolainen
Jens Pomoell
Affiliation:
Department of Physics, University of HelsinkiP.O. Box 64, 00014 University of Helsinki, Finland email: jens.pomoell@helsinki.fi, rami.vainio@helsinki.fi
Rami Vainio
Affiliation:
Department of Physics, University of HelsinkiP.O. Box 64, 00014 University of Helsinki, Finland email: jens.pomoell@helsinki.fi, rami.vainio@helsinki.fi
Silja Pohjolainen
Affiliation:
Department of Physics and Astronomy, University of Turku, Tuorla Observatory, 21500 Piikkiö, Finland email: silpoh@utu.fi
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Abstract

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We study the MHD processes related to a flare/CME event in the lower solar corona using numerical simulations. Our initial state is an isothermal gravitationally stratified corona with an embedded flux rope magnetic field structure. The eruption is driven by applying an artificial force to the flux rope. The results show that as the flux rope rises, a shock structure is formed, reaching from ahead of the flux rope all the way to the solar surface. The speed of the shock quickly exceeds that of the driving flux rope, and the shock escapes from the driver. Thus, the shock exhibits characteristics both of the driven and blast wave type. In addition, the temperature distribution behind the shock is loop-like, implying that erupting loop-like structures observed in soft X-ray images might be shocks. Finally, we note that care must be taken when performing correlation analysis of the speed and location of type II bursts and ejecta.

Keywords

Sun: coronal mass ejections (CMEs)flaresradio radiation, shock waves, plasmas
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 4 , Symposium S257: Universal Heliophysical Processes , September 2008 , pp. 493 - 495
Copyright
Copyright © International Astronomical Union 2009

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