Hα line emission and infrared excess in Be Stars

dc.contributor.author	Goraya, P. S.
dc.contributor.author	Rautela, B. S.
dc.date.accessioned	2010-03-03T04:47:00Z
dc.date.available	2010-03-03T04:47:00Z
dc.date.issued	1985
dc.identifier.citation	This article is downloaded for ADS	en_US
dc.identifier.uri	http://hdl.handle.net/123456789/594
dc.description.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.	en_US
dc.language.iso	en_US	en_US
dc.relation.ispartofseries	ass113-373
dc.subject	Hα emission - Be Stars	en_US
dc.title	Hα line emission and infrared excess in Be Stars	en_US
dc.type	Article	en_US