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Paper: X-Ray Plasma Temperature Distribution in the Wind of ζ Puppis
Volume: 465, Four Decades of Massive Star Research - A Scientific Meeting in Honor of Anthony J. Moffat
Page: 252
Authors: Hervé, A.; Rauw, G.; Nazé, Y.
Abstract: Different scenarios try to explain the X-ray production in the O-type star wind (magnetic confinement, embedded shocks…) and their plasma temperature distribution. In this context, we have developed a new modeling code which computes synthetic spectra as a function of plasma temperature, abundances, and localization of the X-ray emitting shell in the wind. Then we combine several synthetic spectra in order to fit the observed high-resolution spectra. Our preliminary results on ζ Puppis reveal a non-porous wind as well as non-solar abundances for the CNO elements. More important, an extended region with a low temperature plasma begins to emit close to the star surface while small shells with hotter temperature plasmas emit farther in the wind.
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