  We present a system model for optical and far UV spectra of the nova-like
variable UX UMa involving a white dwarf, secondary star, gas stream, hot spot
and accretion disk using our code BINSYN and based on an initially adopted
system distance. Calculated SED intensity data successfully fit successive
tomographically-extracted annuli longward of the Balmer limit but require a
postulated `iron curtain' shortward of the Balmer limit that is applied to the
annulus section closest to the secondary star, while postulated recombination
emission fills in the model SED shortward of the Balmer limit and is applied to
the annulus section more remote from the secondary star. The same model fits
$UBV$ 1954 light curves by Walker and Herbig. Fits to $HST$ $FOS$ spectra are
approximate but require assumed time-variable changes in the SED. Comparable
effects, possibly involving variable absorption, afflict $FUSE$ spectra.
