  We study in detail the properties of the accreting corona model for active
galactic nuclei and galactic black holes. In this model the fraction of the
energy liberated in the corona at a given radius is calculated from the global
parameters of the model (mass of the central object, accretion rate and
viscosity parameter) and it appears to be a strong function of the radius. The
model predicts the relative decrease of the coronal hard X-ray emission with an
increase of the accretion rate. The presented description of disc/corona
interaction forms a basis for further studies of disc disruption mechanism.
