  We study the accretion flows towards a central Kerr super-spinning attractor,
discussing the formation of the flow inversion points, defined by condition
$u^{\phi}=0$ on the particles flow axial velocity. We locate two closed
surfaces, defining \emph{inversion coronas} (spherical shells), surrounding the
central attractor. The coronas analysis highlights observational aspects
distinguishing the central attractors and providing indications on their spin
and the orbiting fluids.
  The inversion corona is a closed region, generally of small extension and
thickness, which is for the counter-rotating flows of the order of $\lesssim
1.4 M$ (central attractor mass) on the vertical rotational axis.
  There are no co-rotating inversion points (from co-rotating flows). The
results point to strong signatures of the Kerr super-spinars, provided in both
accretion and jet flows. With very narrow thickness, and varying little with
the fluid initial conditions and the emission process details, inversion
coronas can have remarkable observational significance for primordial Kerr
super-spinars predicted by string theory. The corona region closest to the
central attractor is the most observably recognizable and active part,
distinguishing black holes solutions from super-spinars. Our analysis expounds
the Lense--Thirring effects and repulsive gravity effects in the super-spinning
ergoregions.
