  Various generalizations of the scalar, axisymmetric Aretakis "horizon hair"
for extremal black holes have recently appeared in the literature. In this
paper, we present an expression for a non-axisymmetric Aretakis gravitational
charge and its potentially observable imprint at a finite distance from the
horizon (Ori-coefficient) in extremal Kerr black hole backgrounds. We offer
strong and robust numerical evidence for the existence of this hair and its
properties. Specifically, we consider the time evolution of horizon
penetrating, quadrupolar and (subdominant) octupolar gravitational
perturbations with compact support on extremal Kerr (EK) spacetime. We do this
by numerically solving the Teukolsky equation and determining the Aretakis
charge values on the horizon and at a finite distance from the black hole.
