Differences in the heliospheric diffusion coefficients in a model with and without a solar wind termination shock

The inclusion of the solar wind termination shock (TS) in numerical models requires e.g., that the radial perpendicular diffusion coefficient, which dominates cosmic ray modulation in the outer heliosphere, be changed with respect to a situation without a TS. A brief overview of these required changes in the heliospheric diffusion coefficients in models with and without a TS will be given. This will be useful in understanding the effects of the TS on cosmic ray modulation in the heliosphere.