  The UV emission lines of Hercules X-1, resolved with the HST GHRS and STIS,
can be divided into broad (FWHM 750 km/s) and narrow (FWHM 150 km/s)
components. The broad lines can be unambiguously identified with emission from
an accretion disk which rotates prograde with the orbit. The narrow lines,
previously identified with the X-ray illuminated atmosphere of the companion
star, are blueshifted at both phi=0.2 and phi=0.8 and the line flux at phi=0.2
is 0.2 of the flux at phi=0.8. Line ratio diagnostics show that the density of
the narrow line region is log n=13.4+/-0.2 and the temperature is
T=1.0+/-0.2x10^5 K. The symmetry of the eclipse ingress suggests that the line
emission on the surface of the disk is left-right symmetric relative to the
orbit. Model fits to the O V, Si IV, and He II line profiles agree with this
result, but fits to the N V lines suggest that the receding side of the disk is
brighter. We note that there are narrow absorption components in the N V lines
with blueshifts of 500 km/s.
