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Fundamental physical processes in coronae: Waves, turbulence, reconnection, and particle acceleration

Published online by Cambridge University Press:  01 September 2007

Markus J. Aschwanden
Markus J. Aschwanden*
Affiliation:
Laboratory for Solar and Astrophysics, ATC, Lockheed Martin, Bldg. 252, Org. ADBS, Palo Alto, CA 94304, USA email: aschwanden@lmsal.com
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Abstract

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Our understanding of fundamental processes in the solar corona has been greatly progressed based on the space observations of SMM, Yohkoh, Compton GRO, SOHO, TRACE, RHESSI, and STEREO. We observe now acoustic waves, MHD oscillations, turbulence-related line broadening, magnetic configurations related to reconnection processes, and radiation from high-energy particles on a routine basis. We review a number of key observations in EUV, soft X-rays, and hard X-rays that innovated our physical understanding of the solar corona, in terms of hydrodynamics, MHD, plasma heating, and particle acceleration processes.

Keywords

WavesTurbulenceReconnectionParticle Acceleration
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 3 , Symposium S247: Waves & Oscillations in the Solar Atmosphere: Heating and Magneto-Seismology , September 2007 , pp. 257 - 268
Copyright
Copyright © International Astronomical Union 2008

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