  It is shown that rapidly-rotating Kerr black holes are characterized by the
dimensionless ratio $\tau_{\text{gap}}/\tau_{\text{emission}}=O(1)$, where
$\tau_{\text{gap}}$ is the average time gap between the emission of successive
Hawking quanta and $\tau_{\text{emission}}$ is the characteristic timescale
required for an individual Hawking quantum to be emitted from the black hole.
This relation implies that the Hawking cascade from rapidly-rotating black
holes has an almost continuous character. Our results correct some inaccurate
claims that recently appeared in the literature regarding the nature of the
Hawking black-hole evaporation process.
