Kerr black-hole quasinormal frequencies

Black-hole quasinormal modes (QNM) have been the subject of much recent attention, with the hope that these oscillation frequencies may shed some light on the elusive theory of quantum gravity. We compare numerical results for the QNM spectrum of the (rotating) Kerr black hole with an exact formula $\mathrm{Re}\overrightarrow{\omega }{T}_{\mathrm{BH}}\ln 3+\Omega m,$ which is based on Bohr’s correspondence principle. We find a close agreement between the two. The possible implications of this result to the area spectrum of quantum black holes are discussed.