  Recent years have been marked by substantial changes in our understanding of
magnetic turbulence and magnetic reconnection, which, in its turn induced
better understanding of cosmic ray diffusion and acceleration. Current models
of magnetized turbulence are no more ad hoc constructions, but numerically
tested theories. In this very short review we summarize topics presented in two
talks given at the conference and provide a brief sketch of the vast and
rapidly developing field. We discuss how turbulence decreases the efficient
mean free path of the particles in the collisionless plasmas in galaxy clusters
and claim that this makes MHD turbulence description applicable to a wider
range of scales. We discuss the properties of MHD turbulence and its relation
to magnetic reconnection. Finally, we overview how turbulence induces particle
acceleration via second order Fermi process and affects first order Fermi
acceleration in shocks and reconnection regions.
