I will motivate why and how General Relativity can be classically
extended and how black hole solutions in these extensions can differ
from the Schwarzschild and Kerr geometries. I will review how these
differences can be perturbative or non-perturbative according to the
specific extension of General Relativity; how they can appear already
in static configurations or just in time dependent ones (e.g. in
binaries); and how they may even challenge the very notion of black
hole horizon in specific cases. I will also discuss ways to test these
possibilities experimentally, e.g. with gravitational and
electromagnetic detectors.
To begin viewing slides, click on the first slide below. (Or, view as pdf.)