Phase structure of the galactic outflows in both the CRMHD (left) and MHD (right) simulations. We show the probability distribution function of the volume-weighted mass flux ρv_z to highlight gas that is responsible for the mass loss from the galaxy. The top panels show the sound speed (which can also be seen as a proxy for the gas temperature) of gas inside R<30 kpc and 3 kpc<|z|<100 kpc while the bottom panels show the hydrogen number density over outflow velocity v_z. We mark the Mach numbers 0.1, 1, and 10 which can be used to infer that the outflow in both simulations is supersonic. The contour in each panel encloses 75% of the total mass flux. The phase structure of the CRMHD is more diverse and spans multiple orders of magnitude in density while being cooler than the MHD simulation.