Abstract
We apply a finite difference method to the 3D radiative line transfer in accretion disks. The two-level-atom approximation with complete re-distribution is used. As a first step we assume disks which are homogeneous in temperature and pressure. We give monochromatic images of the intensity distribution on the surface of CV disks for several assumptions on the scattering and disk thickness. In the LTE case earlier results (e.g. by Smak, 1969) are confirmed. However, for scattering conditions in thin disks we get a completely different intensity pattern. In a parameter study for geometrically thick disks we show a variety of line profile shapes.
The effect of a corona overlying a disk atmosphere on the Balmer line profiles is studied with a ray tracing technique. Using Stark profile functions and a parametrization of the coronal temperature, we show that the shape of the total profile strongly depends on the structure of the transition zone.
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Adam, J., Innes, D.E., Shaviv, G., Störzer, H., Wehrse, R. (1989). Line Radiation from Stationary Accretion Disks. In: Meyer, F., Duschl, W.J., Frank, J., Meyer-Hofmeister, E. (eds) Theory of Accretion Disks. NATO ASI Series, vol 290. Springer, Dordrecht. https://doi.org/10.1007/978-94-009-1037-9_39
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DOI: https://doi.org/10.1007/978-94-009-1037-9_39
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