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The spectra arising from the disks of nova-like variables show many of thefeatures seen in stellar atmospheres. They are typically modelled either froman appropriated weighted set of stellar atmospheres or a disk atmosphere withenergy is dissipated near the disk plane, with the effective temperaturedistribution expected from a steady state accretion disk. However these modelsgenerally over-predict the depth of the Balmer jump and the slope of thespectrum in the ultraviolet. The problem is likely due to energy dissipation inthe disk atmosphere, which produces a flatter vertical temperature profile thanis observed in stars. Here, we provide validation for this hypothesis in theform of spectra generated using the stellar atmosphere code TLUSTY using aparametric prescription for energy dissipation as a function of depth andclosely match the spectrum of the nova-like IX Vel over the wavelength range1150-6000 \AA.

An Improved Model for the Spectra of Disks of Nova-like Variables