The dynamical evolution of Be disks
In the last years, the viscous decretion disk model (VDDM) came out as the only model capable of reproducing the observed
properties of Be stars. However, this model is still not straightforward to use, particularly because the influence of the stellar
mass loss rate on the disk is still not well understood. Hydrodynamic simulations coupled with radiative tranfer codes now
allow modeling the disk evolution. In this contribution, we discuss some VDDM predictions for the density of the disk for some
simple reference cases and their consequences on photometric observables. We discuss how these predictions compare to
observations, focusing, in particular, on the analysis of Be 28 Cma.