E. I. Chiang and P. Goldreich 1997 ApJ 490 368 doi:10.1086/304869
E. I. Chiang1 and P. Goldreich1
Show affiliationsWe 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 reemits 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.
accretion, accretion disks; circumstellar matter; infrared: stars; radiative transfer; stars: pre-main sequence
Issue 1 (1997 November 20)
Received 1997 March 18, accepted for publication 1997 July 3
E. I. Chiang and P. Goldreich 1997 ApJ 490 368