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On the so-called WO stars

Published online by Cambridge University Press:  25 May 2016

V. Francesco Polcaro ,
Laura Norci ,
Corinne Rossi  and
Roberto Viotti
V. Francesco Polcaro
Affiliation:
Istituto di Astrofisica Spaziale, CNR, Roma, Italy
Laura Norci
Affiliation:
Dunsink Observatory, Castleknock, Dublin, Ireland
Corinne Rossi
Affiliation:
Istituto Astronomico, Universitá La Sapienza, Roma, Italy
Roberto Viotti
Affiliation:
Istituto di Astrofisica Spaziale, CNR, Roma, Italy

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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
Information
Symposium - International Astronomical Union , Volume 193: Wolf-Rayet Phenomena in Massive Stars and Starburst Galaxies , 1999 , pp. 88 - 89
Copyright
Copyright © Astronomical Society of the Pacific 1999 

References

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