  The old novae V533 Her (Nova Her 1963), DI Lac (Nova Lac 1910) and RR Pic
(Nova Pic 1891) are in (or near) their quiescent stage following their nova
explosions and continue to accrete at a high rate in the aftermath of their
explosions. They exhibit continua that are steeply rising into the FUV as well
as absorption lines and emission lines of uncertain origin. All three have FUSE
spectra which offer not only higher spectral resolution but also wavelength
coverage extending down to the Lyman Limit. For DI Lac, we have matched these
FUSE spectra with existing archival IUE spectral coverage to broaden the FUV
wavelength coverage. We adopted the newly determined interstellar reddening
corrections of Selvelli and Gilmozzi (2013). The dereddened FUV spectra have
been modeled with our grids of optically thick accretion disks and hot, NLTE
white dwarf photospheres.
  The results of our modeling analysis indicate that the hot component in RR
Pic and V533 Her is likely to be the accretion disk with a mass accretion of
$10^{-8}M_{\odot}$/yr and $10^{-9}M_{\odot}$/yr respectively. However, the disk
cannot produce the observed absorption lines. For the WD to be the source of
the absorption lines in these two systems, it must be very hot with a radius
several times its expected size (since the WD in these systems is massive, it
has a smaller radius). For DI Lac we find the best fit to be a disk with
$\dot{M}=10^{-10}M_{\odot}$/yr with a 30,000K WD.
