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

Abstract

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 Å.

12 pages, 7 figures

References in corpus (4)

• Gaia Data Release 1. Summary of the astrometric, photometric, and survey properties
• Synthetic NLTE accretion disc spectra for the dwarf nova SS Cyg during an outburst cycle
• TLUSTY User's Guide II: Reference Manual
• The hydrogen Balmer lines and jump in absorption in accretion disc modeling -- an ultraviolet-optical spectral analysis of the dwarf novae UZ Serpentis and CY Lyrae

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• Analysis of accretion disc structure and stability using open code for vertical structure
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