On the importance of the interclump medium for superionization: O VI formation in the wind of ζ puppis

J. Zsargó, D. J. Hillier, J. C. Bouret, T. Lanz, M. A. Leutenegger, D. H. Cohen

Research output: Contribution to journalArticle

29 Citations (Scopus)

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 lowdensity 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. © 2008. The American Astronomical Society.
Original languageAmerican English
JournalAstrophysical Journal
DOIs
StatePublished - 1 Jan 2008
Externally publishedYes

Fingerprint

clumps
void
voids
stellar atmospheres
resonance lines
gases
gas
recombination
x rays
atmosphere
profiles
simulation
code
calculation
material

Cite this

Zsargó, J. ; Hillier, D. J. ; Bouret, J. C. ; Lanz, T. ; Leutenegger, M. A. ; Cohen, D. H. / On the importance of the interclump medium for superionization: O VI formation in the wind of ζ puppis. In: Astrophysical Journal. 2008.
@article{bd1c87381e4047aeae99ee85dfee9f40,
title = "On the importance of the interclump medium for superionization: O VI formation in the wind of ζ puppis",
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 lowdensity 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. {\circledC} 2008. The American Astronomical Society.",
author = "J. Zsarg{\'o} and Hillier, {D. J.} and Bouret, {J. C.} and T. Lanz and Leutenegger, {M. A.} and Cohen, {D. H.}",
year = "2008",
month = "1",
day = "1",
doi = "10.1086/592568",
language = "American English",
journal = "Astrophysical Journal",
issn = "0004-637X",
publisher = "IOP Publishing Ltd.",

}

On the importance of the interclump medium for superionization: O VI formation in the wind of ζ puppis. / Zsargó, J.; Hillier, D. J.; Bouret, J. C.; Lanz, T.; Leutenegger, M. A.; Cohen, D. H.

In: Astrophysical Journal, 01.01.2008.

Research output: Contribution to journalArticle

TY - JOUR

T1 - On the importance of the interclump medium for superionization: O VI formation in the wind of ζ puppis

AU - Zsargó, J.

AU - Hillier, D. J.

AU - Bouret, J. C.

AU - Lanz, T.

AU - Leutenegger, M. A.

AU - Cohen, D. H.

PY - 2008/1/1

Y1 - 2008/1/1

N2 - 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 lowdensity 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. © 2008. The American Astronomical Society.

AB - 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 lowdensity 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. © 2008. The American Astronomical Society.

U2 - 10.1086/592568

DO - 10.1086/592568

M3 - Article

JO - Astrophysical Journal

JF - Astrophysical Journal

SN - 0004-637X

ER -