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J. M. Miller, H. L. Marshall, R. A. Remillard, R. Wijnands (MIT), T. Di Matteo (Harvard Univ.), D. Pooley (MIT), W. Cui (Purdue Univ.), A. C. Fabian (Cambridge Univ.), W. H. G. Lewin (MIT)
We present results of a 30 ksec observation of Galactic black hole X-ray binary Cygnus X-1, obtained with the Chandra X-ray Observatory High Energy Transmission Grating Spectrometer at the end of the ``high/soft'' state of Nov.-Dec. 2000. We find a very strong, narrow, Fe I K-alpha emission line at 6.4 keV and examine likely production mechanisms for this line (e.g. companion wind and disk reflection scenarios). We observed a dip in the X-ray flux during which the Fe I K-alpha line is not detected and other aspects of the spectrum change significantly. Below 2.0 keV, we find absorption and emission lines from ionized material, which we discuss within the context of a hot corona and a strong wind from the companion. Taken as a whole, our results show that high-resolution spectroscopy can reveal a great deal about the accretion environments of this and similar systems.
The author(s) of this abstract have provided an email address for comments about the abstract: jmm@space.mit.edu