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On the so-called WO stars
Published online by Cambridge University Press: 25 May 2016
Extract
The Wolf-Rayet WO spectral sequence was introduced by Barlow & Hummer (1982) for four Pop I WR stars with very strong O VI 381 nm doublet emission. At the time, the evolution of very massive stars was poorly known, and their classification was based on phenomenological grounds. Recently, efforts to improve the WO spectral subtype classification are increasing (Kingsburgh et al. 1995; Crowther et al. 1998).
- Type
- Part 1. Basic observational properties of Wolf-Rayet stars and other hot massive stars
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- Copyright © Astronomical Society of the Pacific 1999