Quantitative analysis of resolved X-ray emission line profiles of O stars

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dc.creatorCohen, David H.
dc.creatorLeutenegger, Maurice A.
dc.creatorTownsend, Richard H. D.
dc.date2007-12-06
dc.date.accessioned2026-07-07T08:47:52Z
dc.date.available2026-07-07T08:47:52Z
dc.descriptionBy quantitatively fitting simple emission line profile models that include both atomic opacity and porosity to the Chandra X-ray spectrum of $ζ$ Pup, we are able to explore the trade-offs between reduced mass-loss rates and wind porosity. We find that reducing the mass-loss rate of $ζ$ Pup by roughly a factor of four, to 1.5 \times 10^{-6} M_sun/yr, enables simple non-porous wind models to provide good fits to the data. If, on the other hand, we take the literature mass-loss rate of 6 \times 10^{-6} M_sun/yr, then to produce X-ray line profiles that fit the data, extreme porosity lengths -- of $h_{\infty} \approx 3$ Rstar -- are required. Moreover, these porous models do not provide better fits to the data than the non-porous, low optical depth models. Additionally, such huge porosity lengths do not seem realistic in light of 2-D numerical simulations of the wind instability.
dc.descriptionAppearing in "Clumping in Hot Star Winds," eds. Hamann, Feldmeier, & Oskinova, Potsdam: Univ.-Verl., 2007; 3 pages; 5 color figures
dc.identifierhttps://arxiv.org/abs/0712.1050
dc.identifierhttp://arxiv.org/abs/0712.1050
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/143755
dc.subjectAstrophysics
dc.titleQuantitative analysis of resolved X-ray emission line profiles of O stars
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