Abstract
Be stars form a subclass of B-type stars, where the stars possess gaseous disk-like structures. Historically, the presence of a disk was detected through line emission present in the spectrum, or through IR excess detected in the spectral energy distribution originating from these sources. However, long-baseline interferometry is the only observational method available today that can be used to spatially resolve the circumstellar regions of Be stars using either line or continuum emission from the disks. A sample of key interferometric results that played a major role in supporting the current view of these systems, where commonly flat, rotationally supported disks connected to rapidly rotating stars are quoted as an observational standard are reviewed. Examples of observational work and results from various interferometric instruments including recent work are presented. Possible future directions are also briefly discussed.
