  We have carried out a synthetic spectral analysis of archival IUE spectra of
the old nova V841 Oph (Nova Oph 1848) taken 15 years apart. The spectra reveal
a rising continuum shortward of 1560\AA, a C {\sc iv} P-Cygni profile
indicative of wind outflow associated with disk accretion in one spectrum, a
deep Ly $\alpha$ profile, and strong N {\sc v} (1238\AA, 1242\AA) and O {\sc v}
(1371\AA) wind/coronal absorption lines. Numerous sharp interstellar resonance
lines are also present. A grid of high gravity atmospheres and accretion disk
models, spanning a wide range of inclinations, accretion rates and white dwarf
masses was compared to the de-reddened spectra. We find that, for a steady
state accretion disk model to account for the FUV spectra, the accretion rate
is only $\sim$3 $\times$ 10$^{-11}$ M$_{\sun}$/yr, 147 years after its outburst
in 1848, with an implied distance within $\sim$300 pc. The accretion rate at
147 years post-outburst is smaller than expected for an old nova.
