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Motivated by the recent interest in quantization of black hole area spectrum,we consider the area spectrum of Kerr and extremal Kerr black holes. Based onthe proposal by Bekenstein and others that the black hole area spectrum isdiscrete and equally spaced, we implement Kunstatter's method to derive thearea spectrum for the Kerr and extremal Kerr black holes. The real part of thequasinormal frequencies of Kerr black hole used for this computation is of theform $m\Omega$ where $\Omega$ is the angular velocity of the black holehorizon. The resulting spectrum is discrete but not as expected uniformlyspaced. Thus, we infer that the function describing the real part ofquasinormal frequencies of Kerr black hole is not the correct one. Thisconclusion is in agreement with the numerical results for the highly dampedquasinormal modes of Kerr black hole recently presented by Berti, Cardoso andYoshida. On the contrary, extremal Kerr black hole is shown to have a discretearea spectrum which in addition is evenly spaced. The area spacing derived inour analysis for the extremal Kerr black hole area spectrum is not proportionalto $\ln 3$. Therefore, it does not give support to Hod's statement that thearea spectrum $A_{n}=(4l^{2}_{p}ln 3)n$ should be valid for a genericKerr-Newman black hole.Comment: 10 pages, no figure, LaTeX; v2: 12 pages, clarifying comments and an  Appendix are added, version to appear in Mod. Phys. Lett.

AREA SPECTRUM OF KERR AND EXTREMAL KERR BLACK HOLES FROM QUASINORMAL MODES