Abstract
The rocket spectra taken by Morton et al. (1967) were used as a basis for the investigation. These are in the far ultraviolet region of the Orion supergiants δ, ∊, ζ Orionis. Because of the similarity in spectral type and luminosity of these stars and the great strength of the shifted resonance lines it was possible to derive a mean P Cygni profile (standard error 5 % of the continuum) representing a typical single ultraviolet resonance line for a star of spectral type ~B0, Mv ~ −6.2. This is the ‘observed’ mean profile in Figures 2 and 3.
Sign-in/Register to access full text options 
Talk to us
Join us for a 30 min session where you can share your feedback and ask us any queries you have
Schedule a callDisclaimer: All third-party content on this website/platform is and will remain the property of their respective owners and is provided on "as is" basis without any warranties, express or implied. Use of third-party content does not indicate any affiliation, sponsorship with or endorsement by them. Any references to third-party content is to identify the corresponding services and shall be considered fair use under The CopyrightLaw.
