Abstract
The method of matched asymptotic expansions is used to calculate the detailed structure of white dwarf- accretion disk boundary layers. Both optically thick and thin boundary layers are investigated for various values of the relevant parameters, as long as the layer's vertical extension remains very much smaller than the white dwarf's radius. Detailed, self consistent solutions for the boundary layer's and disk's structure are calculated and used to find the amount of energy, radiated onto the accreting white dwarf (recently recognized to be an important factor in nova outburst modelling).
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