  We study an accretion disc with a hot continuous corona. We assume that the
corona itself accretes and therefore it is powered directly by the release of
the gravitational energy and cooled by radiative interaction with the disc. We
consider the vertical structure of such a corona and show that the radial
infall is accompanied by strong vertical outflow. Such a model has two
important consequences: (i) at a given radius the corona forms only for
accretion rate larger than a limiting value and the fraction of energy
dissipated in the corona decreases with increasing accretion rate, and (ii) the
disc spectra are significantly softer in the optical/UV band in comparison with
the predictions of standard accretion discs due to the mass loss and the
decrease of internal dissipation in the disc. Both trends correspond well to
the mean spectra of radio quiet AGN and observed luminosity states in galactic
black hole candidates.
