Fermionic Quasinormal Spectrum of the Kerr Black Hole

We study {\it analytically} the asymptotic quasinormal spectrum of fermionic fields in the Kerr spacetime. We find an analytic expression for these black-hole resonances in terms of the black-hole physical parameters: its Bekenstein-Hawking temperature $T_{BH}$, and its horizon’s angular velocity $\mathrm{\Omega }$, which is valid in the asymptotic limit $1\ll {\omega }_I\ll {\omega }_R$. It is shown that according to Bohr’s correspondence principle, the emission of a Rarita-Schwinger quantum ($s=3\mathrm{/}2$) corresponds to a fundamental black-hole area change $\mathrm{\Delta }A=4\mathrm{\hslash }\ln 2$, while the emission of a Weyl neutrino field ($s=1\mathrm{/}2$) corresponds to an adiabatic quantum transition with $\Delta A=0$.