Stochastic acceleration by MHD turbulence in Solar flares

Details Stochastic acceleration by MHD turbulence in Solar flares Stochastic acceleration by MHD turbulence in Solar flares

Dec 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007agufmsh23a1157y&link_type=abstract

American Geophysical Union, Fall Meeting 2007, abstract #SH23A-1157

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2114 Energetic Particles (7514), 7514 Energetic Particles (2114)

Scientific paper

We address the problem of particle acceleration in Solar flares. We account for turbulent energy cascade of MHD modes and their damping processes. We consider stochastic acceleration of particles by fast modes. We find that transit time acceleration dominates over the acceleration by gyroresonance. Acceleration rates are obtained with both quasilinear and nonlinear approaches and compared with energy loss rate. Scattering by fast modes appears to be sufficient to prevent the protons from escaping the system during the acceleration. Confinement of electrons, on the other hand, requires the existence of plasma waves. Electrons can be accelerated to GeV energies through the process. We estimate the total energy transferred into non-thermal particles, and show that our approach provides sufficiently accurate results.

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