Anisotropic Diffusion in Galactic Cosmic Ray transport using PICARD
R. Kissmann, O. Reimer*, F. Niederwanger and A.W. Strong
August 16, 2017
August 03, 2018
The Picard code for the numerical solution of the cosmic ray propagation problem is optimised to incorporate the complexity of the 3D structure of our Galaxy down to decaparsec scales. Picard was used to investigate the impact of anisotropic cosmic-ray diffusion on the Galactic cosmic-ray flux distribution. We discuss different magnetic-field models for our Galaxy in the context of a cosmic-ray source distribution aligned with the Galactic spiral arms. With the resulting sets of transport parameters, that can reproduce cosmic-ray observations at Earth for the different magnetic field models, we find restrictions for the spatial diffusion tensor. We show that related variations in the diffusive coupling to the Galactic halo can lead to changes in the cosmic-ray gradients. The most severe changes are found in the Galactic centre where a modification in the magnetic-field topology can change the cosmic-ray proton flux by more than a factor of two.
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