  We present far-ultraviolet (905 -- 1182 A), time-series spectroscopy of the
eclipsing, novalike cataclysmic variable, UX UMa, acquired with FUSE. The
time-averaged spectrum is complex and is dominated by overlapping spectral
features. The most prominent features are emission lines of CIII, NIII}, NIV,
and OVI. They are broad (FWHM >= 1800 km/s) and double-peaked with a central
absorption at zero velocity. During eclipse, the spectrum is simpler: the
emission lines remain bright, but the absorption components of the lines and
the weaker features between the emission lines disappear entirely, leaving a
flat continuum. This behavior is also evident in GHRS (1149 -- 1660 A) spectra
that we retrieved from the HST archive. The FUV spectra show flickering on time
scales of several minutes. The flickering is seen primarily in the continuum
and/or the weaker lines rather than in the prominent emission lines. The
orbital light curve has a dip in the FUV flux between orbital phases 0.45 --
0.65, similar to a pre-eclipse dip detected in HST observations. The EWs of the
line absorption features decrease during the dip. We have detected a systematic
wavelength shift of spectral features on the orbital period, but with a phase
lag of ~ 20 degrees, a phenomenon that has been reported at optical
wavelengths. We discuss the implications of our results in the context of
models of an accretion disk with a chromosphere between the disk and the
extended wind. Finally, we note that the observed FUV flux is too low to be
consistent with the temperature and radius of the WD derived by Baptista et al.
(1995), suggesting that their remaining binary parameters, including a mass
ratio of 1, ought to be viewed with skepticism.
