  Ringed accretion disks (RADs) are aggregates of corotating and
counterrotating toroidal accretion disks orbiting a central Kerr super-massive
Black Hole (SMBH) in AGNs. The dimensionless spin of the central BH and the
fluids relative rotation are proved to strongly affect the RAD dynamics. There
is evidence of a strict correlation between SMBH spin, fluid rotation and
magnetic fields in RADs formation and evolution. Recently, the model was
extended to consider RADs constituted by several magnetized accretion tori and
the effects of a toroidal magnetic field in RAD dynamics have been
investigated. The analysis poses constraints on tori formation and emergence of
RADs instabilities in the phases of accretion onto the central attractor and
tori collision emergence. Magnetic fields and fluids rotation are proved to be
strongly constrained and influence tori formation and evolution in RADs, in
dependence on the toroidal magnetic fields parameters. Eventually, the RAD
frame investigation constraints specific classes of tori that could be observed
around some specific SMBHs identified by their dimensionless spin
