Abstract
Classical Be stars are rapidly rotating, massive stars that exhibit several distinct observational characteristics due to the presence of thin disks of gas concentrated in the stars equatorial plane. In order to understand the mechanisms that govern the development of these circumstellar disks, we use computational codes to create theoretical models of these objects and their environments and we compare the predicted observables to observations of Be stars. The primary focus of this work is the comparison of different approaches used in the creation of theoretical Be star models. We examine independently developed non-local thermodynamic equilibrium (NLTE) codes designed to model circumstellar environments by simultaneously solving the problems of radiative transfer, thermal equilibrium and statistical equilibrium. A detailed analysis of the differences and similarities between different radiative transfer techniques may provide valuable insight into the physical processes which govern the development of Be star circumstellar disks.
