Influence of Radiative Transfer on the Vertical Structure of Accretion Disks
A brief review of various theoretical approaches to model accretion disks is presented. Emphasis is given to models that determine self-consistently the structure of a disk together with the radiation field. It is argued that a proper treatment of the vertical structure is essential for calculating theoretical spectra to be compared with observations. It is demonstrated that neither the blackbody nor model stellar atmosphere fluxes provide a satisfactory approximation of the emergent radiation. Finally, several models calculated with various degree of sophistication in treatment of interaction of radiation with matter, and with different values of viscosity, are intercompared, and possible diagnostic consequences are briefly discussed.
KeywordsOptical Depth Vertical Structure Accretion Disk Effective Temperature Central Star
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