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We present simulations of the transport of fast particles through three-dimensional turbulent magnetic field configurations. A time dependency is imposed on the plane wave modes used in constructing these fields such than acceleration via the second-order Fermi process is possible. We consider simulations of models with low and high turbulence levels for non-relativistic waves. The predictions of quasi-linear theory are discussed with respect to the simulation data. We conclude that for pure stochastic acceleration via Alfvén waves to be plausible as the generator of UHECR in Cen A, the baryon number density would need to be several orders of magnitude below currently held upper-limits.
O'Sullivan, S., Reville, B. & Taylor, A. (2010). Relativistic Particle Acceleration in Tangled Magnetic Fields. Numerical Modeling of Space Plasma Flows, Astronum-2009. 29 June-3 July 2009, Chamonix, France. pg.33. doi:10.21427/5j84-5563