Cosmic rays play an important role in young stellar objects. In the inner regime, cosmic rays impinging upon circumstellar disks provide an important source of ionization, and play an important role in disk evolution and planet formation. On a larger scale, these cosmic rays must propagate inward through the magnetic fields of the protostellar envelope, where these fields tend to have hour-glass shapes. On both of these scales, incoming cosmic rays are affected by a variety of physical processes, including modulation by turbulent magnetic fields. Globally, these fields naturally provide both a funneling effect, where cosmic rays from larger volumes are focused into smaller regions, and a magnetic mirroring effect, where cosmic rays are repelled due to the increasing field strength. This talk considers cosmic ray propagation in the presence of turbulent magnetic fields, both on the larger scale where the field has an hour-glass morphology and on the smaller scale where the field takes a spiral form (roughly analogous to that produced by the Solar wind). To address this problem, we construct new coordinate systems where one coordinate follows the magnetic field lines and consider magnetic perturbations to the field in the perpendicular directions. The presence of magnetic turbulence replaces the mirroring points with a distribution of values and moves the mean location outward. Our results thus help quantify the degree to which cosmic ray fluxes are reduced in young stellar objects.