Spatially resolved line profiles across the simulation area at solar disk center illustrate how the convective blueshift in the field-free case gradually changes into a magnetic redshift. From left to right, the weak Fe I 683.7006 nm and strong Fe I 524.7050 nm lines are shown (at the same pixels in the same snapshot) from simulations with fields = 0, 120, and 240 mT (0, 1200, 2400 G). The nonmagnetic convective blueshift is caused by large, bright, and blueshifted granules dominating over spatially narrow, dark, and redshifted downflows. In the magnetic case, the surface areas of up- and downflows are more equal, the velocities are lower, while the redshifted contributions from small bright elements bias the average.