  We derive hydrostatic, radiative equilibrium models for passive disks
surrounding T Tauri stars. Each disk is encased by an optically thin layer of
superheated dust grains. This layer re-emits directly to space about half the
stellar energy it absorbs. The other half is emitted inward and regulates the
interior temperature of the disk. The heated disk flares. As a consequence, it
absorbs more stellar radiation, especially at large radii, than a flat disk
would. The portion of the spectral energy distribution contributed by the disk
is fairly flat throughout the thermal infrared. At fixed frequency, the
contribution from the surface layer exceeds that from the interior by about a
factor 3 and is emitted at more than an order of magnitude greater radius.
Spectral features from dust grains in the superheated layer appear in emission
if the disk is viewed nearly face-on.
