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Infrared (1.4–4.1μM) Spectra of Wolf-Rayet Stars

Published online by Cambridge University Press:  14 August 2015

P. M. Williams
P. M. Williams*
Affiliation:
United Kingdom Infrared Telescope Unit of the Royal Observatory Edinburgh 900 Leilani Street Hilo, Hawaii 96720

Abstract

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The spectra of a variety of Wolf-Rayet stars have been observed with ∼1% spectral resolution in the 1.4–4.1μm region using UKIRT. Strong lines due to ions of helium and carbon are observed and their relative strengths discussed. The He I singlet at 2.058μm is anomalously strong relative to other He I lines in WC stars and is responsible for the difference in the (H-K) colours of WN and WC stars. Emission line corrections to H, K and L magnitudes of different types are discussed. The Sanduleak 0 VI star ST 3 shows very strong C IV lines like the WC5 stars but not the strong He I.

Type
SESSION 1 — THE WOLF-RAYET PHENOMENON
Information
Symposium - International Astronomical Union , Volume 99: Wolf-Rayet Stars: Observations, Physics, Evolution , 1982 , pp. 73 - 78
Copyright
Copyright © Reidel 1982 

References

Allen, D.A., Harvey, P.M. & Swings, J.P., 1972. Astr. Astrophys., 20, p. 333.Google Scholar
Edlén, B., 1956. Vistas in Astronomy, 2, p. 1456.Google Scholar
Kuhi, L.V., 1966. Ap. J., 145, p. 715.Google Scholar
Sanduleak, N., 1971. Ap. J. Lett., 164, p. L71.Google Scholar
Thompson, R.I. and Tokunaga, A.T., 1980. Ap. J., 235, p. 889.CrossRefGoogle Scholar
Williams, P.M. and Allen, D.A., 1980. Observatory, 100, p. 202.Google Scholar
Williams, P.M., Adams, D.J., Arakaki, S., Beattie, D.H., Born, J., Lee, T.J., Robertson, D.J. and Stewart, J.M., 1980. MNRAS, 192, p. 25P.Google Scholar