  Q Cygni (Nova Cygni 1876) is the third oldest old novae (after WY Sge and
V841 Oph) with a long orbital period of 10.08 hours and spectroscopic
peculiarities in the optical including the presence of variable wind outflow
revealed by optical P Cygni profiles in the HeI lines and H alpha beta (Kafka
et al. 2003). We have carried out a synthetic spectral analysis of a far
ultraviolet IUE archival spectrum of Q Cygni using our optically thick, steady
state, accretion disk models and model white dwarf photospheres. We find that
the accretion light of a luminous accretion disk dominates the FUV flux of the
hot component with a rate of accretion 2-3 1.E-9 Msun/yr. We find that Q Cygni
lies at a distance of 741 \pm 110 pc . The implications of our results for
theoretical predictions for old novae are presented.
