Evaporation of a Kerr-black-bounce by emission of scalar particles

Understand

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 $a_* \sim 0.555$.