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[113.05U] X-ray Emission Line Profile Modeling of O stars: zeta Puppis as a Wind-Shock Source

R. H. Kramer, D. H. Cohen (Swarthmore College), S. P. Owocki (Bartol Research Institute, University of Delaware)

The origin of X-ray emission lines associated with O- and B-type stars is the subject of continuing controversy. Leading theories point to shocks in the star's massive, radiation-driven winds as the source of the X-rays. In recent years \textit{Chandra} has taken high-resolution X-ray spectra of several hot stars, revealing broad and often asymmetric line profiles. At the same time, theoretical calculations of line profiles from spherically-symmetric shock distributions in the wind have shown the potential to produce similar profile shapes. We have parameterized a spherically-symmetric, distributed-shock wind model and fit it to several lines from the O4f star \zeta Puppis. Our fits suggest lower than expected X-ray continuum opacities, and onset of shock formation within a few stellar radii.

The author(s) of this abstract have provided an email address for comments about the abstract: roban+aas@sccs.swarthmore.edu

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Bulletin of the American Astronomical Society, 34, #4
© 2002. The American Astronomical Soceity.