  The spectra arising from the disks of nova-like variables show many of the
features seen in stellar atmospheres. They are typically modelled either from
an appropriated weighted set of stellar atmospheres or a disk atmosphere with
energy is dissipated near the disk plane, with the effective temperature
distribution expected from a steady state accretion disk. However these models
generally over-predict the depth of the Balmer jump and the slope of the
spectrum in the ultraviolet. The problem is likely due to energy dissipation in
the disk atmosphere, which produces a flatter vertical temperature profile than
is observed in stars. Here, we provide validation for this hypothesis in the
form of spectra generated using the stellar atmosphere code TLUSTY using a
parametric prescription for energy dissipation as a function of depth and
closely match the spectrum of the nova-like IX Vel over the wavelength range
1150-6000 \AA.
