  Motivated by novel results in the theory of black-hole quantization, we study
{\it analytically} the quasinormal modes (QNM) of ({\it rotating}) Kerr black
holes. The black-hole oscillation frequencies tend to the asymptotic value
$\omega_n=m\Omega+i2\pi T_{BH}n$ in the $n \to \infty$ limit. This simple
formula is in agreement with Bohr's correspondence principle. Possible
implications of this result to the area spectrum of quantum black holes are
discussed.
