  The problem of accelerating cosmic rays is one of fundamental importance,
particularly given the uncertainty in the conditions inside the acceleration
sites. Here we examine Diffusive Shock Acceleration in arbitrary turbulent
magnetic fields, constructing a new model that is capable of bridging the gap
between the very weak ($\delta B/B_0 \ll 1$) and the strong turbulence regimes.
To describe the diffusion we provide quantitative analytical description of the
"Bohm exponent" in each regime. We show that our results converge to the well
known quasi-linear theory in the weak turbulence regime. In the strong regime,
we quantify the limitations of the Bohm-type models. Furthermore, our results
account for the anomalous diffusive behaviour which has been noted previously.
Finally, we discuss the implications of our model in the study of possible
acceleration sites in different astronomical objects.
