The evolution of magnetohydrodynamic turbulence resulting from magnetic reconnection will be investigated, and subsequently employed to evaluate the transport and acceleration of energetic particles in solar flares. The cascade of turbulent energy from large to small scales and its dissipative damping through the heating and acceleration of particles determine the evolution of the plasma fluctuations. The transport coefficients for the electrons and protons follow from the coupling to the fluctuations, and enter into a Fokker-Planck equation describing the energy spectrum and pitch-angle distribution of the superthermal particles. Incorporation of these results into a coupled and self-consistent solar flare model will provide specific predictions that can be tested against ground, and space-based observations.
