Evolution of our simulations. In each column we show edge-on maps of the column density for one simulation at three different times: t = 0.5, 1.0, and 1.5 Gyr. In the last row, we also show the face-on view of the column density at t = 1.5 Gyr. The simulations with an initially smaller magnetic field develop much larger star-forming disks due to the weaker magnetic support. The inclusion of CRs leads to a more fluffed up disk as the CRs diffuse out and drives a galactic outflow that is stronger in the initially weak-field model CRMHD-low.