Document Type

Conference Proceeding

Publication Date

4-1-2008

Published In

Clumping In Hot-Star Winds: Proceedings Of An International Workshop

Abstract

By 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∞≈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.

Editor(s)

W.-R. Hamann, A. Feldmeier, and L. M. Oskinova

Conference

International Workshop On Clumping In Hot-Star Winds

Conference Dates

June 18-22, 2007

Conference Location

University Of Potsdam, Potsdam, Germany

Comments

This work is a preprint retrieved from arXiv.org at arXiv:0712.1050
The published version of this work is available from Universität Potsdam.

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