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Q Cygni (Nova Cygni 1876) is the third oldest old novae (after WY Sge andV841 Oph) with a long orbital period of 10.08 hours and spectroscopicpeculiarities in the optical including the presence of variable wind outflowrevealed by optical P Cygni profiles in the HeI lines and H alpha beta (Kafkaet al. 2003). We have carried out a synthetic spectral analysis of a farultraviolet IUE archival spectrum of Q Cygni using our optically thick, steadystate, accretion disk models and model white dwarf photospheres. We find thatthe accretion light of a luminous accretion disk dominates the FUV flux of thehot component with a rate of accretion 2-3 1.E-9 Msun/yr. We find that Q Cygnilies at a distance of 741 \pm 110 pc . The implications of our results fortheoretical predictions for old novae are presented.

The Amazing Old Nova Q Cygni: A Far Ultraviolet Synthetic Spectral Analysis