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

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 l = 0.99r+. We compare the results with a Kerr black hole evaporating under the same conditions. First, we compute the graybody factors and show that the Kerr-black-bounce evolves toward a non-Schwarzschild-like asymptotic state with a* -0.47, differently from a Kerr black hole whose asymptotic spin would be a* -0.555. We show that this result depends on the combined contributions of the changes in the graybody factors and in the surface gravity introduced 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 by exploiting its Hawking emission.

Automated summary

We study the evaporation of a regular rotating black hole 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 l = 0.99r+. We compare the results with a Kerr black hole evaporating under the same conditions. Our findings show that the regular black hole evolves to a non-Schwarzschild-like state with a slightly different asymptotic spin compared to a Kerr black hole. We also discuss how the surface gravity affects the temperature and primary emissivity, resulting in a longer lifetime for the regular black hole. Finally, we briefly comment on the possibility of investigating the beyond-the-horizon structure of a black hole through its Hawking emission.