We have computed theoretical models of circumstellar disks for the classical Be stars κ Dra, β Psc, and υ Cyg. Models were constructed using a non-LTE radiative transfer code developed by Sigut & Jones (2007), which incorporates a number of improvements over previous treatments of the disk thermal structure, including a realistic chemical composition. Our models are constrained by direct comparison with long-baseline optical interferometric observations of the Hα-emitting regions and by contemporaneous Hα line profiles. Detailed comparisons of our predictions with Hα interferometry and spectroscopy place very tight constraints on the density distributions for these circumstellar disks.
- Circumstellar matter
- Stars: emission-line, Be
- Stars: individual (κ Dra, β Psc, υ Cyg)
- Techniques: interferometric