  The role of MHD turbulence in the cosmic ray acceleration process in a volume
with a reconnecting magnetic field is studied by means of Monte Carlo
simulations. We performed modelling of proton acceleration with the 3D analytic
model of stationary reconnection of Craig et al. (1995) providing the
unperturbed background conditions. Perturbations of particle trajectories due
to a turbulent magnetic field component were simulated using small-amplitude
pitch-angle momentum scattering, enabling modelling of both small and large
amplitude turbulence in a wide wave vector range. Within the approach, no
second-order Fermi acceleration process is allowed. Comparison of the
acceleration process in models involving particle trajectory perturbations to
the unperturbed one reveals that the turbulence can substantially increase the
acceleration efficiency, enabling much higher final particle energies and flat
particle spectra.
