  A well-established phenomenon in general relativity is the dragging of
inertial frames by a spinning object. In particular, due to the dragging of
inertial frames by a ring orbiting a central black hole, the angular-velocity
of the black-hole horizon in the composed black-hole-ring system is no longer
related to the black-hole angular-momentum by the simple Kerr-like (vacuum)
relation
$\Omega^{\text{Kerr}}_{\text{H}}(J_{\text{H}})=J_{\text{H}}/2M^2R_{\text{H}}$.
Will has performed a perturbative treatment of the composed black-hole-ring
system in the regime of slowly rotating black holes and found the explicit
relation
$\Omega^{\text{BH-ring}}_{\text{H}}(J_{\text{H}}=0,J_{\text{R}},R)=2J_{\text{R}}/R^3$
for the angular-velocity of a central black hole with zero angular-momentum.
Analyzing a sequence of black-hole-ring configurations with adiabatically
varying (decreasing) circumferential radii, we show that the expression found
by Will implies a smooth transition of the central black-hole angular-velocity
from its asymptotic near-horizon value
$\Omega^{\text{BH-ring}}_{\text{H}}(J_{\text{H}}=0,J_{\text{R}},R\to
R^{+}_{\text{H}})$ to its final Kerr (vacuum) value
$\Omega^{\text{Kerr}}_{\text{H}}(J^{\text{new}}_{\text{H}})$. We use this
important observation in order to generalize the result of Will to the regime
of black-hole-ring configurations in which the central black holes possess
non-zero angular momenta. Remarkably, we find the simple universal relation
$\Delta\Omega_{\text{H}}\equiv\Omega^{\text{BH-ring}}_{\text{H}}(J_{\text{H}},J_{\text{R}},R\to
R^{+}_{\text{H}})-\Omega^{\text{Kerr}}_{\text{H}}(J_{\text{H}})={{J_{\text{R}}}/{4M^3}}$
for the asymptotic deviation of the black-hole angular-velocity in the composed
black-hole-ring system from the corresponding angular-velocity of the
unperturbed (vacuum) Kerr black hole with the same angular-momentum.
