  We investigate ringed accretion disks constituted by two tori (rings)
orbiting on the equatorial plane of a central super-massive Kerr black hole. We
discuss the emergence of the instability phases of each ring of the
macro-configuration (ringed disk) according to Paczynski violation of
mechanical equilibrium. In the full general relativistic treatment, we consider
the effects of the geometry of the Kerr spacetimes relevant in the
characterization of the evolution of these configurations. The discussion of
the rings stability in different spacetimes enables us to identify particular
classes of central Kerr attractors in dependence of their dimensionless spin.
As a result of this analysis we set constraints of the evolutionary schemes of
the ringed disks related to the tori morphology and their rotation relative to
the central black hole and to each other. The dynamics of the unstable phases
of this system is significant for the high energy phenomena related to
accretion onto super-massive black holes in active galactic nuclei (AGNs), and
the extremely energetic phenomena in quasars which could be observable in their
X-ray emission.
