Abstract
We present solutions for the radial and vertical structure of standard accretion disks (Shakura & Sunyaev). In these disks, the accretion and distribution of the angular momentum are controlled by the viscosity parameter, α. Self-similarity solutions for accretion disks predict that α must be constant on the disk, if the viscosity can be described by a power law ν ∝ R^{γ} with γ = 1. Recently, Isella et al. (2009) showed that for a sample of 14 young stellar objects, -0.8 ≤ γ ≤ 0.8, indicating that α = α (R). Based on these evidences, we have computed the structure for 11 of these objects, using α (R) as prescribed by Isella et al. (2009). We compare our results with the solutions of the same disks for α =10^{-3} to 10^{-1}, constant. Our results show that the disks (as expected) are lighter, cooler and thinner in its inner regions, when compared with the disks with α constant. We make a qualitative analysis of the solutions obtained with the JED + SAD models (Jet Emitting Disk + Standard Accretion Disk), which also predict the same behavior for the central part of the accretion disks. We show that the height scale maps the age of the objects: the disks become thinner overall to the extent as the objects become older. As the stars studied have different masses and accretion rates, the results appear to be independent of the specific characteristics of the disk+star system.
