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The extreme P-Cygni star HDE 316285

Published online by Cambridge University Press:  25 May 2016

D. John Hillier ,
Paul A. Crowther ,
Francisco Najarro de la Parra  and
Alexander W. Fullerton
D. John Hillier
Affiliation:
Department of Physics and Astronomy, University of Pittsburgh, 3941 O'Hara Street, Pittsburgh, PA 15260, USA
Paul A. Crowther
Affiliation:
University College, London, England
Francisco Najarro de la Parra
Affiliation:
CSIC, Madrid, Spain
Alexander W. Fullerton
Affiliation:
The Johns Hopkins University, Baltimore, USA

Abstract

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New line-blanketed models for the P-Cygni star HDE 316285 have been calculated. Representative model atoms for H, He I, He II, Ca I, Ca II, Mg I, Mg II, Al II, Al III, Fe II, and Fe III are included in the calculations. We confirm the basic parameters derived by Hillier et al. (1998) in an earlier unblanketed study, and also confirm that many of the optical metal lines are produced by continuum fluorescence. The charge exchange reaction Fe2+ + H ⇌ Fe+ + H + modifies the Fe ionization structure and significantly enhances the strength of the optical Fe II emission lines.

Type
Part 2. Models for single star evolution of massive stars: wind + atmosphere + interior
Information
Symposium - International Astronomical Union , Volume 193: Wolf-Rayet Phenomena in Massive Stars and Starburst Galaxies , 1999 , pp. 246 - 247
Copyright
Copyright © Astronomical Society of the Pacific 1999 

References

Hillier, D.J., Crowther, P.A., Najarro, F., Fullerton, A.W. 1998, A&A 340, 483 Google Scholar
Hillier, D.J., Miller, D.L. 1998, ApJ 496, 407 Google Scholar
Najarro, F., Hillier, D. J., Stahl, O. 1997, A&A 326, 1117 Google Scholar
Neufeld, D.A., Dalgarno, A. 1987, Phys. Rev. A. 35, 3142 CrossRefGoogle Scholar