The 0.1-2.5-KEV X-Ray Spectrum of the O4F-STAR Zeta-Puppis

Details The 0.1-2.5-KEV X-Ray Spectrum of the O4F-STAR Zeta-Puppis The 0.1-2.5-KEV X-Ray Spectrum of the O4F-STAR Zeta-Puppis

Sep 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993a%26a...276..117h&link_type=abstract

Astronomy and Astrophysics, Vol.276, NO. 1/SEPI, P. 117, 1993

Astronomy and Astrophysics

Astrophysics

97

Stars: Individual: Ζ Pup, Stars: Early-Type, Stars: Mass-Loss, X-Rays: Stars

Scientific paper

We have obtained a high quality ROSAT PSPC spectrum of the bright O4f star ζ Pup. Allowing for the wind X-ray opacity, as computed from detailed non-LTE stellar wind models of ζ Pup, and under the assumption that the X-rays arise from shocks distributed throughout the wind, we have been able to match the observed X-ray spectrum (0.1 to 2.5keV).
The best model fit is obtained when He++ recombines to He+ in the outer regions of the stellar wind, as predicted by recent detailed cool wind model calculations. With a single temperature plasma, the best model fit indicates a temperature of log Ts(K) = 6.5 to 6.6 corresponding to shock velocities of around 500 km s-1. A 2 temperature plasma yields a significantly improved fit, and indicates temperatures of log Ts(K) = 6.2 and 6.7 for the 2 components. The hotter component accounts for 55% of the intrinsic (75% of the observed) X-ray flux. Due to absorption by the stellar wind, and to a minor extent stellar occultation, less than 5% of the total emitted X-ray flux escapes the star. The models require significant X-ray emission (particularly at energies less than 0.5 keV) from large radii (r > 100R*).
In models without recombination, the fits, even with a 2 temperature plasma, are unacceptable. A significant K shell absorption is predicted by these models, but is definitely not present in the observational data. The analysis suggests that the X-ray flux provides an invaluable diagnostic of the ionization of helium in the stellar wind of stars with low reddening.

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