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IR Spectroscopy of WN Stars

Published online by Cambridge University Press:  14 August 2015

J.D. Hillier
J.D. Hillier*
Affiliation:
Mount Stromlo and Siding Spring Observatories The Australian National University Canberra, Australia

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The combination of IR data with radio, optical and UV observations has the potential to greatly increase our understanding of the WR phenomena. Consequently we are obtaining IR spectra from 1.1 to 4.2µ for a sample of southern WN stars (K < 7th magnitude) using a low resolution, R∼100, circular variable filter wheel (CVF) and a cooled grating spectrometer, (CGS) (Jones et al. 1981) with a maximum resolution of 2000. Previous IR spectral studies of WR stars have generally concentrated on line identification, and beyond 1.7µ they have been limited to low resolution (Barnes et al. 1974, Cohen et al. 1978, Williams et al. 1980). With the CGS it is now possible to obtain spectra at resolutions sufficiently high to split blends and reveal details of line profiles. Below we present preliminary results of our observations.

Type
SESSION 3 — MASS-LOSS FROM WR STARS: OBSERVATIONS AND THEORY
Information
Symposium - International Astronomical Union , Volume 99: Wolf-Rayet Stars: Observations, Physics, Evolution , 1982 , pp. 225 - 229
Copyright
Copyright © Reidel 1982 

References

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