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The interacting symbiotic binary star, CI Cygni, is a system which consists of a hot star orbiting a red giant. Matter from the larger star is being transfered to the smaller one. Both IUE and more recently, the Goddard High Resolution Spectrograph on HST have detected variable ultraviolet emission lines produced by this transfer. Phase-dependent changes to the doppler velocity of the matter allow us to map the direction of the flow. Using the HST snd IUE spectrometers, we re-examined two different types of lines (resonance and intercombination) which had been reported to show velocity differences. We will present an analysis of these data showing the relative locations of high and low density features in the matter transfer in this system. The lead authors are pleased to acknowledge partial support for this effort through NASA grant NAG5-2368 to the University of Denver.
