Physical conditions in Wolf-Rayet atmospheres

Bappu, M. K. V

dc.contributor.author	Bappu, M. K. V
dc.date.accessioned	2006-04-08T06:33:47Z
dc.date.available	2006-04-08T06:33:47Z
dc.date.issued	1957-10
dc.identifier.citation	Bulletin of the National Institute of Sciences of India, No. 9, pp. 155-162	en
dc.identifier.uri	http://hdl.handle.net/2248/878
dc.description.abstract	A critical discussion of present-day knowledge regarding the Wolf-Rayet atmosphere is presented. It is shown that the large widths usually ascribed to the emission lines are formed by heavy blending, and that the individual components are in many cases seen distinctly on high dispersion coude spectra. Arguments are given to show that the single stars alone do not yield observational information of the exact dynamical conditions in the atmosphere. The results obtained from the binary systems V444 Cygni and CQ Cephei are discussed.
dc.format.extent	1543101 bytes
dc.format.mimetype	application/pdf
dc.language.iso	en	en
dc.subject	Wolf-Rayet atmospheres	en
dc.title	Physical conditions in Wolf-Rayet atmospheres	en
dc.type	Article	en