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Title:
On the Importance of the Interclump Medium for Superionization: O VI Formation in the Wind of ζ Puppis
Authors:
Zsargó, J.; Hillier, D. J.; Bouret, J.-C.; Lanz, T.; Leutenegger, M. A.; Cohen, D. H.
Affiliation:
AA(Department of Physics and Astronomy, University of Pittsburgh, 3941 O'Hara Street, Pittsburgh, PA 15260; .), AB(Department of Physics and Astronomy, University of Pittsburgh, 3941 O'Hara Street, Pittsburgh, PA 15260; .), AC(Laboratoire d'Astrophysique de Marseille, CNRS-Université de Provence, 13388 Marseille cedex 13, France.), AD(Department of Astronomy, University of Maryland, College Park, MD 20742.), AE(Goddard Space Flight Center, 8800 Greenbelt Road, Greenbelt, MD 20771.; NASA Postdoctoral Fellow.), AF(Department of Physics and Astronomy, Swarthmore College, 500 College Avenue, Swarthmore, PA 19081.)
Publication:
The Astrophysical Journal, Volume 685, Issue 2, pp. L149-L152. (ApJL Homepage)
Publication Date:
10/2008
Origin:
UCP
ApJ Keywords:
Stars: Early-Type, Stars: Winds, Outflows, X-rays: individual (ζ Puppis), X-Rays: Stars
DOI:
10.1086/592568
Bibliographic Code:
2008ApJ...685L.149Z

Abstract

We have studied superionization and X-ray line formation in the spectra of ζ Pup using our new stellar atmosphere code (XCMFGEN) that can be used to simultaneously analyze optical, UV, and X-ray observations. Here, we present results on the formation of the O VI λλ1032, 1038 doublet. Our simulations, supported by simple theoretical calculations, show that clumped wind models that assume void in the interclump space cannot reproduce the observed O VI profiles. However, enough O VI can be produced if the voids are filled by a low-density gas. The recombination of O VI is very efficient in the dense material, but in the tenuous interclump region an observable amount of O VI can be maintained. We also find that different UV resonance lines are sensitive to different density regimes in ζ Pup: C IV is almost exclusively formed within the densest regions, while the majority of O VI resides between clumps. N V is an intermediate case, with contributions from both the tenuous gas and clumps.
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