Physics
Scientific paper
Dec 2004
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004agufmsh13a1149m&link_type=abstract
American Geophysical Union, Fall Meeting 2004, abstract #SH13A-1149
Physics
7514 Energetic Particles (2114), 7519 Flares, 7554 X Rays, Gamma Rays, And Neutrinos, 7867 Wave/Particle Interactions
Scientific paper
We present initial results from a unified and self-consistent model of particle acceleration and atmospheric response in impulsive solar flares. In our model, electrons and ions are stochastically energized from thermal to relativistic energies on short timescales by cascading MHD turbulence, which is assumed to have been excited initially in the coronal region of a flare loop during the primary energy release phase. The accelerated particles then propagate to the denser transition region and chromosphere, where they can deposit a large fraction of their energy and drive the formation of a hydrodynamic shock that propagates back into the corona. The density enhancements that accompany this shock in turn modify the particle acceleration process in the corona. The two main components of the simulation are the NRL Dynamic Solar Flux Tube Model code and a spatially-dependent quasilinear particle acceleration/wave evolution code. We demonstrate through these realistic simulations that stochastic acceleration by MHD turbulence is able to account for all the major features of solar flare energetic particles. This work was supported by NASA grant NAG5-12794.
Mariska John T.
Miller Aaron J.
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