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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, noting that blackholes can have three types of resonance modes which are quasinormal modes(QNM), total transmission modes (TTM), and total reflection modes (TRM), wepropose that all of these modes in highly damped regime should be used inquantizing the black hole. Although the QNM and the TTM of the Kerr black holegive us complicated quantization conditions from the Bohr-Sommerfeldquantization of action variable, we find a very simple result from the TRM. Itgives equally spaced outer horizon area. Therefore by Bekenstein-Hawking arealaw we find that the Kerr black hole has universal behavior of the equallyspaced entropy spectrum. With the same argument, we find that theReissner-Nordstrom black hole also has equally spaced entropy spectrum.

Entropy spectra of black holes from resonance modes in scattering by the black holes