The universal relaxation bound suggests that the relaxation times of perturbed thermodynamical systems is bounded from below by the simple time-times-temperature (TTT) quantum relation $\tau\times T\geq { { \hbar}\over{ \pi}}$. It is known that some perturbation modes of near-extremal Kerr black holes in the regime $MT_{ \text{ BH}}/\hbar\ll m^{ -2}$ are characterized by normalized relaxation times $\pi\tau\times T_{ \text{ BH}}/\hbar$ which, in the approach to the limit $MT_{ \text{ BH}}/\hbar\to0$, make infinitely many oscillations with a tiny constant amplitude around $1$ and therefore cannot be used directly to verify the validity of the TTT bound in the entire parameter space of the black-hole spacetime (Here $\{ T_{ \text{ BH}},M\}$ are respectively the Bekenstein-Hawking temperature and the mass of the black hole, and $m$ is the azimuthal harmonic index of the linearized perturbation mode). In the present compact paper we explicitly prove that all rapidly-spinning Kerr black holes respect the TTT relaxation bound. In particular, using analytical techniques, it is proved that all black-hole perturbation modes in the complementary regime $m^{ -1}\ll MT_{ \text{ BH}}/\hbar\ll1$ are characterized by relaxation times with the simple dimensionless property $\pi\tau\times T_{ \text{ BH}}/\hbar\geq1$.
Categories: gr-qc astro-ph.HE hep-th