  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
$\Omega$, 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 ($s=3/2$) corresponds to a fundamental black-hole
area change $\Delta A=4\hbar \ln 2$, while the emission of a Weyl neutrino
field ($s=1/2$) corresponds to an adiabatic quantum transition with $\Delta
A=0$.
