Constraints on hot star X-ray source characteristics from combinded analysis of X-ray and UV observations

Details Constraints on hot star X-ray source characteristics from combinded analysis of X-ray and UV observations Constraints on hot star X-ray source characteristics from combinded analysis of X-ray and UV observations

Nov 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994ap%26ss.221..287m&link_type=abstract

Astrophysics and Space Science (ISSN 0004-640X), vol. 221, no. 1-2, p. 287-294

Astronomy and Astrophysics

Astronomy

Hot Stars, Stellar Mass, Stellar Physics, Stellar Spectra, Stellar Winds, Ultraviolet Astronomy, X Ray Astronomy, X Ray Sources, H Alpha Line, Mass Distribution, Photosphere, Shock Waves, Stellar Models, Ultraviolet Spectra, X Ray Spectra

Scientific paper

Results from wind ionization calculations are presented which show how the P-Cygni profiles of 'superionized' species such as O VI can provide information about the X-ray source characteristics of early-type stars. Using detailed radiative and atomic physics models, we find that a significant source of X-ray emission from zeta Pup comes from a region in the wind located within rougly 1 to 2 stellar radii of the photosphere. Our results suggest that X-rays sources in which emission occurs exclusively at large radii (r greater than or approximately equal to a few R*) are inconsistent with UV P-Cygni profiles for O VI. Instead, we find that X-ray emission from shocks distributed throughout the lower regions of the wind (r approximately equal to 1-2 R*) is consistent with both X-ray and UV data, as well as mass loss rates deduced from radio and H-alpha observations.

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