Modeling the Structure of Hot Star Disks: a Critical Evaluation of the Viscous Decretion Scenario

Abstract

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 ($α$-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 $δ$ Scorpii. Our results confirm that a viscous decretion disk model is consistent with these observations.