  There is a growing set of observational data demonstrating that cosmic rays
exhibit small-scale anisotropies (5-30 deg) with amplitude deviations lying
between 0.01-0.1 percent that of the average cosmic ray flux. A broad range of
models have been proposed to explain these anisotropies ranging from
finite-scale magnetic field structures to dark matter annihilation. The
standard diffusion transport methods used in cosmic ray propagation do not
capture the transport physics in a medium with finite-scale or coherent
magnetic field structures. Here, we present a Monte Carlo transport method,
applying it to a series of finite-scale magnetic field structures to determine
the requirements of such fields in explaining the observed cosmic
ray,small-scale anisotropies.
