We study particle transport in the solar corona in the presence of magnetic fluctuations. We perform numerical simulations by injecting particles at the center of a model coronal loop, and by varying the turbulence correlation length λ, the turbulence level, and the particle energy. For large λ, the ratio between the Larmor radius and turbulence wavelength is small, and the magnetic moment is conserved. In this case, a fraction of the injected particles is trapped by magnetic mirroring in the magnetic loop near the injection region. The rest of the particles propagates freely along Β, corresponding to ballistic transport. Decreasing λ, that is increasing the ratio ρ/λ, the magnetic moment is no more well conserved, and pitch angle diffusion progressively sets in. Parallel transport changes progressively from ballistic to superdiffusive, and finally, for small λ, to diffusive. Perpendicular transport may also exhibit superdiffusive and subdiffusive behaviour.
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