Astronomy and Astrophysics – Astrophysics
Scientific paper
Jun 2006
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006sf2a.conf..533d&link_type=abstract
SF2A-2006: Proceedings of the Annual meeting of the French Society of Astronomy and Astrophysics Eds.: D. Barret, F. Casoli, G.
Astronomy and Astrophysics
Astrophysics
Scientific paper
Particle accelerated in solar flares draw their energy from the magnetic field. The dissipative scale of the magnetic energy in the solar corona implies that the magnetic energy is transmitted to the particles through a large number of dissipative regions (DR). Although not directly observed, the magnetic energy release process is assumed to evolve in a SOC state which leads to a power-law behaviour of the spectrum of the energy released in each DR. We present an approach to link the magnetic energy release to the acceleration process that occurs in each DR to finally compute the particle energy distribution. We consider that each accelerated particle leaves the acceleration region after one interaction but we introduce a distribution of the particle acceleration lengths inside each acceleration region. We finally compare our different results with particle energy distributions deduced from solar flare observations and we discuss the assumptions of the model.
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