Abstract:
The Hα observations of a selected sample of bright Be stars are presented. The available infrared observations at K band (2.2 µm) of these stars have been used to find the infrared excess emission. The analysis of the combined data show that Lҥα, the luminosity of the Hα emission line, is proportional to Liʀ and Lҥα shows that both the infrared excess and the Hα line originate in a common region. It is also detected that the infrared excess emission is produced throughout the whole envelop whereas the Hα is emitted in some defined region of the circumstellar (CS) envelop.
