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There is a growing set of observational data demonstrating that cosmic raysexhibit small-scale anisotropies (5-30 deg) with amplitude deviations lyingbetween 0.01-0.1 percent that of the average cosmic ray flux. A broad range ofmodels have been proposed to explain these anisotropies ranging fromfinite-scale magnetic field structures to dark matter annihilation. Thestandard diffusion transport methods used in cosmic ray propagation do notcapture the transport physics in a medium with finite-scale or coherentmagnetic field structures. Here, we present a Monte Carlo transport method,applying it to a series of finite-scale magnetic field structures to determinethe requirements of such fields in explaining the observed cosmicray,small-scale anisotropies.

Cosmic Ray transport in mixed magnetic fields and their role on the observed anisotropies