Silicon Ion Fluorescence Spectra in Vela X-1 and Cygnus X-3

Details Silicon Ion Fluorescence Spectra in Vela X-1 and Cygnus X-3 Silicon Ion Fluorescence Spectra in Vela X-1 and Cygnus X-3

Apr 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002aps..aprx11003l&link_type=abstract

American Physical Society, April Meeting, Jointly Sponsored with the High Energy Astrophysics Division (HEAD) of the American As

Astronomy and Astrophysics

Astrophysics

Scientific paper

Using the Chandra HETG, we have detected a set of spectrally isolated features in Vela X-1 and Cygnus X-3, which we identify as Si K-alpha line complexes from a broad range of charge states. The fluorescing gas is likely to be an overdense, X-ray irradiated component of a cloudy stellar wind formed and maintained by a host of instabilities. In support of spectral analyses of these data, we have performed new atomic level population kinetics calculations relevant to K-alpha emission, and examined the effects of resonant Auger destruction, an important radiative transfer process. Our results indicate a rich ion to ion variation in the spectral properties of what is traditionally treated as a monolithic ``K line.'' We show that the complexity of these emission features can be turned to our advantage, as it provides the basis for a novel set of spectroscopic diagnostics of both the local plasma conditions and the large-scale distribution of reprocessing gas.

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