  We consider agglomerates of misaligned tori orbiting a supermassive black
hole. The aggregate of tilted tori is modeled as a single orbiting
configuration by introducing a leading function governing the distribution of
toroids (and maximum pressure points inside the disks) around the black hole
attractor. The orbiting clusters are composed by geometrically thick, pressure
supported, perfect fluid tori. This analysis places constraints on the
existence and properties of tilted tori and more general aggregates of orbiting
disks. We study the constraints on the tori collision emergence and the
instability of the agglomerates of tori with general relative inclination
angles, the possible effects of the tori geometrical thickness and on the
oscillatory phenomena. Some notes are discussed on the orbiting ringed
structure in dependence of the dimensionless parameter ${\xi}$ representing the
(total) BH rotational energy extracted versus the mass of the BH, associating
${\xi}$ to the characteristics of the accretion processes.
