Abstract
A large amount of the energy released during solar flares is converted into high energy particle acceleration: electrons and ions. These particles are detected either in the interplanetary space or through the radiations that they produce in the solar atmosphere (radio, X-ray and γ-ray emissions). After a brief discussion of the hard X-ray and γ-ray emission processes, we focus on the observational constraints on the accelerated particles: occurrence of ion acceleration in solar flares, time scale for particle acceleration, transport from the acceleration site to the emitting regions. The relative abundances of the accelerated nuclei and in the interaction site deduced from γ-ray spectroscopy are discussed. Finally the relationship between gamma-ray line and solar energetic events will be examined.
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