The spectra arising from the discs 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 disc atmosphere with energy is dissipated near the disc plane, with the effective temperature distribution expected from a steady-state accretion disc. However, these models generally overpredict 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 disc 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.

中文翻译：

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类新星变星盘光谱的改进模型

由类新星变量圆盘产生的光谱显示了恒星大气中的许多特征。它们通常是从一组适当加权的恒星大气中模拟出来的，或者是在盘面附近耗散能量的盘状大气，其有效温度分布来自稳态吸积盘。然而，这些模型通常高估了巴尔默跳跃的深度和紫外光谱的斜率。这个问题很可能是由于圆盘大气中的能量耗散造成的，这会产生比在恒星中观察到的更平坦的垂直温度分布。这里，