Speaker
Description
Black holes are one of the most intriguing and puzzling objects in the universe. Computing the volume of a black hole is not as straightforward as defining the area of the enclosing horizon. In this article we define the volume using the technique developed by Christodoulou and Rovelli for Schwarzschild black holes and extend it to the case of a rotating black hole in 2+1 dimensions. We show that the maximum contribution to the volume of the hyper-surface comes from what we call the steady state radius. We then find that this volume grows linearly and indefinitely with the advance time. We then introduce a scalar field in this maximal hyper-surface and compute its entropy. We find that in the near extremal limit, the entropy of this scalar field is proportional to the horizon entropy of the black hole.
| Session | Formal Theory |
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