  Since the Bekenstein's proposal that a black hole has equally spaced area
spectrum, the quasinormal modes as the characteristic modes of a black hole
have 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 was
inconsistent with the Bekenstein's proposal. In this paper, noting that black
holes can have three types of resonance modes which are quasinormal modes
(QNM), total transmission modes (TTM), and total reflection modes (TRM), we
propose that all of these modes in highly damped regime should be used in
quantizing the black hole. Although the QNM and the TTM of the Kerr black hole
give us complicated quantization conditions from the Bohr-Sommerfeld
quantization of action variable, we find a very simple result from the TRM. It
gives equally spaced outer horizon area. Therefore by Bekenstein-Hawking area
law we find that the Kerr black hole has universal behavior of the equally
spaced entropy spectrum. With the same argument, we find that the
Reissner-Nordstrom black hole also has equally spaced entropy spectrum.
