Accretion Disks around Young Objects. I. The Detailed Vertical Structure

We discuss the properties of an accretion disk around a star with parameters typical of classical T Tauri stars (CTTSs) and with the average accretion rate for these disks. The disk is assumed steady and geometrically thin. The turbulent viscosity coefficient is expressed using the α prescription, and the main heating mechanisms considered are viscous dissipation and irradiation by the central star. The energy is transported by radiation, turbulent conduction, and convection. We find that irradiation from the central star is the main heating agent of the disk, except in the innermost regions, R < 2 AU. The irradiation increases the temperature of the outer disk relative to the purely viscous case. As a consequence, the outer disk (R > 5 AU) becomes less dense, optically thin, and almost vertically isothermal, with a temperature distribution T ~ R^-1/2. The decrease in surface density at the outer disk decreases the disk mass by a factor of 4 with respect to a purely viscous case. In addition, irradiation tends to make the outer disk regions stable against gravitational instabilities.