Density-averaged radial profile of the fluid parameters for different resolutions at an early time (t = 250 Myr α_B = 0.5). From top to bottom we have: the Prandtl number, the magnetic Reynolds number and the regular Reynolds number. The Prandtl number seem to be largely independent of the resolution and mainly be effected by the conditions within the galaxy (supersonic + shear + stratified environment). Both the magnetic and regular Reynolds number can be seen to increase with a factor of 4 as we increase the resolution, which is in agreement with the expected second order of the numerical diffusion.