  We study a regular rotating black hole evaporating under the Hawking emission
of a single scalar field. The black hole is described by the Kerr-black-bounce
metric with a nearly extremal regularizing parameter $\ell=0.99r_+$. We compare
the results with a Kerr black hole evaporating under the same conditions.
Firstly, we compute the gray-body factors and show that the Kerr-black-bounce
evolves towards a non-Schwartzchild-like asymptotic state with $a_* \sim 0.47$,
differently from a Kerr black hole whose asymptotic spin would be $a_* \sim
0.555$. We show that this result depends on the combined contributions of the
differences in the gray-body factors and the surface gravity affected by the
regularizing parameter. We also discuss how the surface gravity affects the
temperature and the primary emissivity and decreases those quantities with
respect to the Kerr black hole. Consequently, the regular black hole has a
longer lifetime. Finally, we briefly comment on the possibility of
investigating the beyond-the-horizon structure of a black hole exploiting its
Hawking emission.
