Orateur
Description
We are entering an era of high-precision measurements of black holes, either through gravitational waves (LVK, and soon LISA) or direct imaging (EHT). It is therefore interesting to study black hole spacetimes within both General Relativity (GR) and alternative theories, to confront them with observations. In GR, the Kerr spacetime, which describes rotating black holes, is the most general astrophysically relevant solution. However, in modified gravity theories, very few rotating solutions are known, even though real black holes always possess non-zero spin. Finding exact rotating solutions is known to be a very complicated task, but approximate analytical solutions can be obtained in the slow-rotation regime. Here, we present a general method to compute first-order slowly rotating black holes in a class of modified theories of gravity.
