  How and where cosmic rays are produced, and how they diffuse through various
turbulent media, represent fundamental problems in astrophysics with far
reaching implications, both in terms of our theoretical understanding of
high-energy processes in the Milky Way and beyond, and the successful
interpretation of space-based and ground based GeV and TeV observations. For
example, recent and ongoing detections, e.g., by Fermi (in space) and HESS (in
Namibia), of $\gamma$-rays produced in regions of dense molecular gas hold
important clues for both processes. In this paper, we carry out a comprehensive
numerical investigation of relativistic particle acceleration and transport
through turbulent magnetized environments in order to derive broadly useful
scaling laws for the energy diffusion coefficients.
