The X-ray Spectrum and Global Structure of the Stellar Wind in VELA X-1

Details The X-ray Spectrum and Global Structure of the Stellar Wind in VELA X-1 The X-ray Spectrum and Global Structure of the Stellar Wind in VELA X-1

Apr 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999head....4.3803s&link_type=abstract

American Astronomical Society, HEAD meeting #4, #38.03; Bulletin of the American Astronomical Society, Vol. 31, p.741

Astronomy and Astrophysics

Astronomy

Scientific paper

The ASCA eclipse spectrum of Vela X-1 exhibits two distinct sets of discrete features: (1) recombination lines and radiative recombination continua from mostly hydrogenic and helium-like species produced by photoionization in an extended stellar wind; and (2) fluorescent K-shell lines associated with near-neutral species also present in the circumsource medium. The presence of emission lines from these two extreme degrees of ionization states cannot be explained by emission originating from a smooth stellar wind alone. Through a detailed differential emission measure analysis of the Vela X-1 spectrum, we find that a model in which hundreds of cool clumps are embedded in a hotter, more ionized gas can account for the observed line spectrum. Most of the wind mass is contained in the clumps, while most of the wind volume (>95%) is occupied by the highly ionized component.

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