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Line Strengths in WN Stars

Published online by Cambridge University Press:  14 August 2015

E. Myckky Leep
E. Myckky Leep*
Affiliation:
Joint Institute for Laboratory Astrophysics, University of Colorado and National Bureau of Standards Boulder, Colorado 80309∗

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We have analyzed high-dispersion spectra of over 100 WN stars in the Galaxy and the Large Magellenic Cloud (LMC). Most of the spectra were obtained through 4-m telescopes (Conti, Leep, and Perry 1981). The measured strengths of the WN classification lines N III λλ4634-41, N IV λ4057, N V λ4604 (Smith 1968) for stars of WN subtypes 2.5–8 are shown in Figure 1. The assignments of WN subtypes are based on visual estimates of ratios of line strengths according to the scheme of Smith (1968), except that stars appearing to be earlier than WN3 are classified as WN2 or WN2.5 as explained by vander Hucht et al. (1981) and by Conti, Leep and Perry (1981).

Type
SESSION 1 — THE WOLF-RAYET PHENOMENON
Information
Symposium - International Astronomical Union , Volume 99: Wolf-Rayet Stars: Observations, Physics, Evolution , 1982 , pp. 41 - 45
Copyright
Copyright © Reidel 1982 

References

Beals, C.S.: 1938, Trans. IAU 6, p. 248.Google Scholar
Conti, P.S., Leep, E.M., and Perry, D.: 1981, submitted to Astrophys. J. vander Hucht, K.A., Conti, P.S., Lundström, I., and Stenholm, B.: 1981, Space Science Reviews 28, p. 227.Google Scholar
Smith, L.F.: 1968, Monthly Notices Roy. Astron. Soc. 138, p. 109.Google Scholar