Astronomy and Astrophysics – Astrophysics
Scientific paper
Jan 2001
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001stin...0132281m&link_type=abstract
Technical Report, Prism Computational Sciences Madison, WI United States
Astronomy and Astrophysics
Astrophysics
High Temperature Plasmas, X Ray Spectra, Ultraviolet Radiation, Spectral Resolution, Early Stars, Resonance Lines, Embedding, X Ray Astrophysics Facility, X Ray Sources, Radiation Distribution, Stellar Winds
Scientific paper
High-resolution X-ray spectra have recently been obtained using the Chandra X-ray Satellite Observatory for the two hot supergiant stars zeta Pup and delta Ori. The spectra show the presence of strong K-shell line emission from O, Ne, Mg, Si, and S, as well as strong L-shell line emission from Fe. Initial examination of the spectra indicates that the lines are significantly broader than what would be expected for a stationary plasma, and appear to be consistent with Doppler-broadened emission from hot plasma forming in shock-heated regions embedded in the wind (see Figure 1). Chandra has sufficient spectral resolution to study the velocity structure of isolated X-ray line profiles. Our analysis for zeta Pup has shown blue-shifted and skewed line profiles, providing the most direct evidence that the X-ray source is embedded in the stellar wind. The sensitivity of the He-like fir (forbidden-intercombination-resonance) lines to a strong UV radiation field is used to estimate the radial distances at which lines of O VII, Ne IX, Mg XI, Si XIII, and S XV originate.
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