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Since the Bekenstein's proposal that a black hole has equally spaced areaspectrum, the quasinormal modes as the characteristic modes of a black holehave been used in obtaining the horizon area spectrum of the black hole.However, the area spectrum of the Kerr black hole in some previous works wasinconsistent with the Bekenstein's proposal. In this paper, we notice that theKerr black hole has three types of resonance modes which are quasinormal modes(QNM), total transmission modes (TTM), and total reflection modes (TRM). All ofthese resonances represent highly damped oscillations and only depend on theblack hole parameters which are mass, charge and angular momentum of the blackhole. We propose that all of these modes should be used in quantizing the blackhole. With all these modes, we find that both the inner and outer horizon areasof the Kerr black hole are equally spaced. Similar behavior is also found inthe Reissner-Nordstrom black hole.

Quantization of horizon areas of the Kerr black hole