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The Hydrogen Abundances in WN Stars

Published online by Cambridge University Press:  03 August 2017

W.-R. Hamann ,
G. DüNNEBEIL ,
U. Wessolowski  and
W. Schmutz
W.-R. Hamann
Affiliation:
1Institut für Theoretische Physik und Sternwarte der Universität, Olshausenstraße 40, D-2300 Kiel, Federal Republic of Germany
G. DüNNEBEIL
Affiliation:
1Institut für Theoretische Physik und Sternwarte der Universität, Olshausenstraße 40, D-2300 Kiel, Federal Republic of Germany
U. Wessolowski
Affiliation:
1Institut für Theoretische Physik und Sternwarte der Universität, Olshausenstraße 40, D-2300 Kiel, Federal Republic of Germany
W. Schmutz
Affiliation:
2Joint Institute for Laboratory Astrophysics, University of Colorado Boulder, Colorado 80309-0440, USA

Extract

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Hydrogen abundances in WN stars have been derived by Conti et al. (1983) from a “semiquantitative” study of the Balmer-Pickering decrement. No clear correlation between hydrogen detection and spectral subtype could be established: stars with hydrogen and stars without detectable hydrogen are found among both, the WNE (“early”) as well as the WNL (”late”).

Type
Session II. Atmospheres
Information
Symposium - International Astronomical Union , Volume 143: Wolf–Rayet Stars and Interrelations with other Massive Stars in Galaxies , 1991 , pp. 100
Copyright
Copyright © Kluwer 1991 

References

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