New Insights into the X-ray Sources in Hot Star Winds

Details New Insights into the X-ray Sources in Hot Star Winds New Insights into the X-ray Sources in Hot Star Winds

Sep 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001tysc.confe.131m&link_type=abstract

Two Years of Science with Chandra, Abstracts from the Symposium held in Washington, DC, 5-7 September, 2001, meeting abstract.

Computer Science

Normal Stars And White Dwarfs

Scientific paper

The HETG X-ray emission-line spectra of hot stars have revealed a suprising diversity of characteristics. Although all the early-type stars we have observed have shown extremely broad emission lines (≈ 500-1000 km s-1 HWHM), only ζ Puppis has shown the line-centroid blue-shifting expected from wind optical depth effects. Using helium-like ion line diagnostics, it appears that the hardest X-rays in both ζ Pup and ζ Ori originate close to their photospheres, a region where it would be difficult to form strong shocks. The hard X-ray emission from δ Ori originates from a distance roughly corresponding to its close companion star, so binary wind effects are discussed as a possible additional X-ray source.

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