  The Kazakov-Solodukhin black hole metric represents a spherically symmetric
deformation of the Schwarzschild solution due to quantum-gravity corrections.
Assuming the absence of nonspherical deformations of the metric, this problem
was solved nonperturbatively. In this study, we investigate the intensity of
Hawking radiation in the background of such quantum-corrected black holes and
the behavior of their quasinormal modes (QNM). Our findings indicate that while
the geometry and such classical characteristics as the fundamental QNM
frequencies or the shadow radius are only slightly altered, the Hawking
radiation and the frequencies of QNM overtones of sufficiently small black
holes change much more significantly. This Hawking radiation enhancement arises
due to much larger grey-body factors, while the Hawking temperature remains
unaffected. The effect becomes significant at the latest stage of black hole
evaporation.
