Fundamental Physical Processes in Coronae: Waves, Turbulence, Reconnection, and Particle Acceleration
Astrophysics
2009-11-13 v1
Abstract
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.
Cite
@article{arxiv.0711.0007,
title = {Fundamental Physical Processes in Coronae: Waves, Turbulence, Reconnection, and Particle Acceleration},
author = {Markus J. Aschwanden},
journal= {arXiv preprint arXiv:0711.0007},
year = {2009}
}
Comments
Proc. IAU Symp. 247, Waves and Oscillations in the Solar Atmosphere: Heating and Magneto-Seismology, (ed. R. Erdelyi)