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H. Yan, A. Lazarian (UW-Madison), V. Petrosian (Stanford U)
We consider a model in which kinetic energy released by Solar flares at large scale is being transported by a turbulent cascade to small scales and accelerates ions and electrons. The turbulent cascade considered is MHD cascade and we use the recent insights in the properties of MHD turbulence to calculate the efficiency of energy transport to small scales. We compare rates for the damping arising from ion-ion collisions, collisionless dampings and also the feed back of nonthermal particles to the rates of non-linear cascading of slow, fast and Alfven modes to determine the scales at which the cascades of those modes will be truncated and the energy is transfered into heat. We calculate acceleration of ions and electrons by MHD perturbation taking into account both resonance interactions and transient time damping. We find that fast modes are most efficient in the acceleration process, while the interaction of the accelerating particles with the anisotropic Alfven modes is marginal. We formulate and solve coupled equations that govern both the turbulence cascade and the acceleration of charged particles to get a self-consistent picture of acceleration. The results of this study are to be compared with Solar flare observations.
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Bulletin of the American Astronomical Society, 37 #2
© 2005. The American Astronomical Soceity.