Abstract
A theoretical study of the properties of the inner boundary layer in an accretion disc is presented. The requirement of causality is shown to exclude a wide range of solutions, some of which are extensively discussed in recent investigations, and to allow for a considerable simplification of the relevant equations. The traditional estimate of the boundary layer thickness, relying on the implicit assumption of nonaxisymmetry, is found to be wrong, and a correct estimate involving the meridional velocity components is derived. It is proven that spatial variability of viscosity is a necessary condition for the existence of a narrow boundary layer
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