We present SOFIA/FORCAST images of S106 at the wavelengths 19, 25, 31, and 37 microns. We use these images to produce color temperature and optical depth maps in order to analyze the warm (~ 60 - 150 K) dust component. We resolve the disk shadow region into several relatively cool (~ 60 - 78 K) lanes with a radially dependent temperature gradient and warmer (~ 75 - 85 K) pockets of dust with a more uniform temperature distribution. The warmer pockets are spatially correlated with pockets of polycyclic aromatic hydrocarbon and HI emission as seen in the images presented by Smith et al. (2001). These results indicate that the disk is clumpy or contains holes with relatively higher UV throughput than the most obscuring parts. We also combine the SOFIA data with data from Spitzer/IRAC (3.6 - 8.0 microns), Herschel/PACS (70 and 160 microns), and the literature to produce the infrared spectral energy distributions of dust at locations in the disk shadow, bipolar lobes, compact sources, and the southwestern edge of the photodissociation region. From the SEDs and radiative transfer modeling, we constrain the mass abundances and size distributions of PAHs and dust grains such as silicates, carbonaceous grains, and very small, transiently heated grains, in these dramatically different regions.