X-Ray Emission-Line Profiles of Three Early-Type Stars Observed with Chandra

Details X-Ray Emission-Line Profiles of Three Early-Type Stars Observed with Chandra X-Ray Emission-Line Profiles of Three Early-Type Stars Observed with Chandra

Feb 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007pasj...59..237y&link_type=abstract

Publications of the Astronomical Society of Japan, Vol.59, No.1, pp.237-244

Astronomy and Astrophysics

Astronomy

2

Stars: Individual (Ζ Puppis, Δ Orionis, Τ Scorpii), Stars: Wind, X-Rays: Spectra, X-Rays: Star

Scientific paper

We analyzed the X-ray emission-line profiles of three early-type stars (ζ Pup, δ Ori, and τ Sco) obtained with Chandra. A phenomenological model, where X-ray sources are distributing in wind above some lower limit radius, can fit the line profiles of ζ Pup and δ Ori; however, the fitting requires a much smaller absorption than expected from the mass-loss rate. This suggests that, if this phenomenological model represents the real X-ray emission region, there is substantial ionization or clumping of the stellar wind. The parameters derived from the line profile of τ Sco indicate that the X-ray-emitting plasma is concentrated on the stellar surface, suggesting the existence of a confined plasma on the stellar surface.

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