  In this paper, we consider angular momentum fluctuations of a Schwartzschild
black hole in thermal equilibrium with radiation which, for the sake of
simplicity is here modeled by a scalar field. Important, we do not set the
black hole angular momentum $J$ identically to zero at the outset; we allow it
to have a small value (in the sense that $J/M<<1$) and then study the
conditions for thermodynamical equilibrium; only then take the $J\rightarrow 0$
limit. We calculate the black hole's angular momentum fluctuations which turn
out to have two independent contributions: one that comes from the black hole
itself, with no respect to the radiation, and another one that arises from the
radiation. The result is astonishingly simple: the radiation contribution
depends exclusively on the cut-off proper distance from the horizon (or
equivalently, the width of the brick wall), while the black hole contribution
is proportional to its event horizon area. Accordingly, there are no strictly
static black holes in nature, they randomly rotate in all possible directions.
Since a black hole is nothing but geometry, we are dealing with geometry
fluctuations -- our results are of quantum-gravitational nature (albeit at a
semi-classical level). Interestingly enough, if we apply to the black hole
fluctuations component the (quantum) rules of angular momentum we obtain an
event horizon area quantization rule, albeit with a different spectrum from an
equally spaced area spectrum which is widely accepted in the literature.
