As Fig. 6 for low‐mass flux disks that flare uniformly: ﹩z=0﹩, 9/8, and 5/4 (﹩H_{d}\propto r^{z}﹩). (a) Relative disk thickness. (b) Temperature profiles. Dashed lines indicate disk‐to‐disk reprocessing calculations for which no stellar source is included. A significant fraction of the reprocessed energy at large radii in the uniformly flaring models comes from photons originating in the disk. (c) Spectral energy distributions. Asterisks indicate the stellar contribution. Spectra are not power law and tend to be double humped with a second peak at the wavelength that corresponds (through the Wien law) to the temperature at the outer edge of the disk.