Calculations for the anisotropic diffusion of protons in the milky way

The distribution of cosmic ray protons in our Galaxy on long timescales is of fundamental physical interest, especially in the context of ''Interstellar-Terrestrial Relations''. The long-term variation of the cosmic ray flux and its implications for the climate on Earth is a major issue in this discussion. In this talk we present results of our modeling in cosmic ray transport. In particular, we incorporate anisotropic diffusion into the numerical solution to the well-known Parker transport-equation. This approach has already been successfully applied to various heliophysical problems and we are now transferring our knowledge to galactic scale. There, the Parker equation can also be extended to include energy losses due to pion production. Important inputs to the physical model are various recent results from theory and observational astronomy on galactic magnetic field structure, galactic winds, cosmic ray sources and diffusion parameters.