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On the Baldwin effect of He II emission lines in WR (WN) stars

van Gent, J. I. and Lamers, H. J. G. L. M. and de Koter, A. and Morris, P. W. (2001) On the Baldwin effect of He II emission lines in WR (WN) stars. Astronomy & Astrophysics, 372 (3). pp. 963-980. ISSN 0004-6361. doi:10.1051/0004-6361:20010534.

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We investigate the relation between the equivalent width of He ii emission lines and the monochromatic continuum luminosity at the line wavelength in the spectra of Wolf-Rayet stars. Model stellar atmospheres and spectra are used to show that the equivalent width inversely correlates with the monochromatic continuum luminosity. We find the effect in Wolf-Rayet star models over a large range of stellar parameters. The effect is shown to be connected to density differences among Wolf-Rayet star winds. The conclusion is drawn that the Baldwin effect may provide a new method for the determination of Wolf-Rayet star distances.

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Additional Information:© 2001 ESO. Article published by EDP Sciences. Received 24 July 2000; Accepted 6 April 2001; Published online 15 June 2001. AdK acknowledges support from NWO Pionier grant 600-78-333 to L.B.F.M. Waters and from NWO Spinoza grant 08-0 to E.P.J. van den Heuvel. We thank Dr. Richard Ignace for his useful comments and suggestions.
Group:Infrared Processing and Analysis Center (IPAC)
Funding AgencyGrant Number
Nederlandse Organisatie voor Wetenschappelijk Onderzoek (NWO)600-78-333
Nederlandse Organisatie voor Wetenschappelijk Onderzoek (NWO)08-0
Subject Keywords:stars: atmospheres - stars: emission line - stars: Wolf-Rayet
Issue or Number:3
Record Number:CaltechAUTHORS:20180307-075500068
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Official Citation:On the Baldwin effect of He ii emission lines in WR (WN) stars. J. I. van Gent, H. J. G. L. M. Lamers, A. de Koter and P. W. Morris. A&A, 372 3 (2001) 963-980. DOI:
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:85159
Deposited By: Tony Diaz
Deposited On:07 Mar 2018 17:36
Last Modified:15 Nov 2021 20:26

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