Speaker
Description
The classification of equilibrium black hole solutions is a fundamental problem in General Relativity. In four spacetime dimensions this is essentially answered by the black hole uniqueness theorem, which roughly states that the only asymptotically flat, stationary black hole solution to the vacuum Einstein equations is the Kerr solution. In higher-dimensional spacetimes, there is no such simple uniqueness theorem - this was revealed by the striking discovery of the black ring, a black hole with horizon topology $S^2 \times S^1$. Alongside the spherical topology Myers-Perry black hole (the natural higher dimensional Kerr analogue), this explicitly shows that even vacuum black holes are not uniquely specified by their mass and angular momenta.
So what is known about black holes in five-dimensional GR? In this talk I will give an overview of the situation and briefly discuss a new classification result leading towards a better understanding of a particular class of these solutions.
| Length of talk | 15-25 minutes |
|---|---|
| Would you be interested in receiving feedback on your talk? | Yes |
| Are you happy for your talk to be recorded? | No |
| Will you be pre-recording your talk? | No |
