Hydrogen surface densities of the CRMHD (left) and the MHD (right) simulations at t = 1 Gyr. Both simulations show morphologically similar structures inside their ISM, which consists of various molecular clouds connected by filamentary dense ISM gas in addition to feedback-driven (super-)bubbles rupturing the galactic disk. There is no visually apparent indication of an increased star formation and feedback activity in either of the simulations, which could readily explain the differences in the galactic winds seen in Fig. 1.