Rotating Black Holes in Randall-Sundrum II Braneworlds

We find rotating black hole solutions in the Randall-Sundrum II (RSII) model, by numerically solving a three-dimensional PDE problem using pseudospectral collocation methods. We compute the area and equatorial innermost stable orbits of these solutions. For large black holes compared with the AdS length scale l the black hole exhibits four-dimensional behavior, approaching the Kerr metric on the brane, while for small black holes, the solution tends instead towards a five-dimensional Myers-Perry black hole with a single nonzero rotation parameter aligned with the brane. This departure from exact four-dimensional gravity may lead to different phenomenological predictions for rotating black holes in the RSII model to those in standard four-dimensional general relativity. This Letter provides a stepping stone for studying such modifications.

Automated summary

In this study, rotating black hole solutions in the Randall-Sundrum II (RSII) model are found by numerically solving a three-dimensional PDE problem. The area and equatorial innermost stable orbits of these solutions are computed. The results show that for large black holes compared with the AdS length scale, the black hole behaves as a four-dimensional object approaching the Kerr metric on the brane, while for small black holes, the solution tends to a five-dimensional Myers-Perry black hole with a single nonzero rotation parameter aligned with the brane. This departure from exact four-dimensional gravity in RSII model may lead to different predictions for rotating black holes compared to standard four-dimensional general relativity.