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Radiative acceleration and ultraviolet resonance line profiles in OB supergiants

Published online by Cambridge University Press:  14 August 2015

J. B. Hutchings
J. B. Hutchings*
Affiliation:
Dominion Astrophysical Observatory, Victoria, B.C., Canada

Extract

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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.

Type
Part II: Stellar Line Spectra
Information
Symposium - International Astronomical Union , Volume 36: Ultraviolet Stellar Spectra and Related Ground-Based Observations , 1970 , pp. 232 - 235
Copyright
Copyright © Reidel 1970 

References

Hutchings, J. B.: 1968, Monthly Notices Roy. Astron. Soc. 141, 219 and 329.Google Scholar
Morton, D. C., Jenkins, E. B., and Bohlin, R. C.: 1967, Astrophys. J. 154, 661.Google Scholar