  We present self-consistent solutions for the disk structure of classical Be
stars. Our disk model is hydrostatically supported in the vertical direction
and the radial structure is governed by viscosity ($\alpha$-disks). We perform
three-dimensional non-LTE Monte Carlo simulations to calculate simultaneously
both the equilibrium temperature and Hydrogen level populations and to solve
self-consistently for the density structure of the disk. We discuss the general
properties of the solution for the disk structure and test our model against
observations of $\delta$ Scorpii. Our results confirm that a viscous decretion
disk model is consistent with these observations.
