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Bram Boroson (GSFC), Tim Kallman (GSFC), Saeqa Dil Vrtilek (CfA)
We present phenomenological models for Hercules X-1 based on HST STIS observations in July of 1998. The data support the interpretation that narrow emission lines arise in the X-ray heated face of the normal star, while broad emission lines arise in a Keplerian accretion disk. From eclipse ingress and egress, we map the strength of the emission lines over the face of the disk, and determine the direction of the disk's rotation. The broad lines are not double-peaked and the doublet ratios are not 1:1; we discuss implications of these facts for disk models. We show how with slightly improved S/N, O\,IV line ratio diagnostics could determine the density in the narrow line region.
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