A Far‐Ultraviolet Study of the Nova‐like V794 Aquilae

We present a spectral analysis of the dereddened FUSE and HST/STIS spectraseparately and combined together assuming E(B-V)=0.1 & 0.2. Overall, we findthat the model fits are in much better agreement with the dereddened spectrawhen E(B-V) is large, as excess emission in the longer wavelengths render theslope of the observed spectra almost impossible to fit, unless E(B-V)=0.2 . The best fit accretion disk model is obtained for E(B-V)=0.2 . A single whitedwarf model leads to a rather hot temperature (30,000K < Twd < 55,000Kdepending on the assumptions) but does not provide a fit as good as theaccretion disk model. A combination of a white dwarf plus a disk does not leadto a better fit. The same best fit disk model is consistently obtained whenfitting the FUSE and HST/STIS spectra individually and when combined together,implying therefore that the disk model is the best fit not only in the leastchi2 sense, but also as a consistent solution across a large wavelength span ofobservation. This is not the case with the single white dwarf model fittingwhich leads to a different (and therefore inconsistent) temperature for eachdifferent spectrum FUSE, STIS and FUSE+STIS