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Implications of X-ray Observations for Electron Acceleration and Propagation in Solar Flares View all abstracts by submitter

Amir Caspi   Submitted: 2011-10-28 12:16

High-energy X-rays and gamma-rays from solar flares were discovered just overfifty years ago. Since that time, the standard for the interpretation ofspatially integrated flare X-ray spectra at energies above several tens of keVhas been the collisional thick-target model. After the launch of the ReuvenRamaty High Energy Solar Spectroscopic Imager (RHESSI) in early 2002, X-rayspectra and images have been of sufficient quality to allow a greater focus onthe energetic electrons responsible for the X-ray emission, including theirorigin and their interactions with the flare plasma and magnetic field. Theresult has been new insights into the flaring process, as well as morequantitative models for both electron acceleration and propagation, and for theflare environment with which the electrons interact. In this article we reviewour current understanding of electron acceleration, energy loss, andpropagation in flares. Implications of these new results for the collisionalthick-target model, for general flare models, and for future flare studies arediscussed.

Authors: Gordon D. Holman, Markus J. Aschwanden, Henry Aurass, Marina Battaglia, Paolo C. Grigis, Eduard P. Kontar, Wei Liu, Pascal Saint-Hilaire, Valentina V. Zharkova
Projects: GONG,Hinode/EIS,Hinode/SOT,Hinode/XRT,Nobeyama Radioheliograph,Owens Valley Solar Array,RHESSI,SDO-AIA,SDO-HMI,SDO-EVE,SoHO-EIT,SoHO-MDI,SoHO-CDS,SoHO-LASCO,SoHO-SUMER,STEREO,TRACE

Publication Status: Published -- Holman, G. D., et al. 2011, Space Sci. Rev., 159, 107; DOI 10.1007/s11214-010-9680-9
Last Modified: 2011-11-17 14:18
Go to main E-Print page  Properties of Energetic Ions in the Solar Atmosphere from γ-Ray and Neutron Observations  An Observational Overview of Solar Flares  Edit Entry  Download Preprint  Delete Entry 

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