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Infrared Spectroscopy of Southern P Cygni Stars

Published online by Cambridge University Press:  04 August 2017

P.J. McGregor ,
A.R. Hyland  and
D.J. Hillier
P.J. McGregor
Affiliation:
Mount Stromlo and Siding Spring Observatories, The Australian National University, Australia
A.R. Hyland
Affiliation:
Mount Stromlo and Siding Spring Observatories, The Australian National University, Australia
D.J. Hillier
Affiliation:
Anglo-Australian Observatory, Australia

Abstract

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Investigations of the 1.0–2.5 μm spectra of high luminosity p Cygni stars reveal the presence of several new emission features. All stars measured show emission in the Brackett and Paschen lines of H I, but the emission strengths of He I 1.083, 1.700, and 2.058 μm relative to the H I lines show large variations. Emission lines of [Fe II] are seen at 1.257 and 1.644 μm in several stars and are particularly strong in HR Car. An interesting subset of these stars show the first-overtone CO bands in emission. The presence of this molecular component associated with hot P Cygni stars has not been inferred from previous optical or UV spectroscopy.

Type
Poster Papers 2
Information
Symposium - International Astronomical Union , Volume 116: Luminous Stars and Associations in Galaxies , 1986 , pp. 257 - 258
Copyright
Copyright © Reidel 1986 

References

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