Let the black-hole geometry be described by a 2D metric

where the metric function has a simple zero at . Assume that this black hole is placed inside a box of finite size so that . In order to get a regular space, one closes the Euclidean time with period , . It is easy to see that Eq. (217) is conformal to the flat disk of radius (): where (), . So that the entanglement entropy of the 2D black hole takes the form [199, 98] where we omit the irrelevant term that is a function of but not of the parameters of the black hole and have retained dependence on the UV regulator .As was shown in [199], the entanglement entropy (219) is identical to the entropy of the thermal atmosphere of quantum excitations outside the horizon in the “brick-wall” approach of ’t Hooft [214].

The black hole resides inside a finite-sized box and is the coordinate of the boundary of the box. The coordinate invariant size of the subsystem complimentary to the black hole is . Two limiting cases are of interest. In the first, the size of the system is taken to infinity. Then, assuming that the black-hole spacetime is asymptotically flat, we obtain that the entanglement entropy (219) approaches the entropy of the thermal gas,

This calculation illustrates an important feature of the entanglement entropy of a black hole placed in a box of volume . Namely, the entanglement entropy contains a contribution of the thermal gas that, in the limit of large volume in dimension , takes the form (7). This is consistent with the thermal nature of the reduced density matrix obtained from the Hartle–Hawking state by tracing over modes inside the horizon.The other interesting case is when is small. In this case, we find the universal behavior

The universality of this formula lies in the fact that it does not depend on any characteristics of the black hole (mass, temperature) other than the value of the curvature at the horizon.Consider two particular examples.

2D de Sitter spacetime is characterized by the metric function and the Hawking temperature . In this spacetime the size of the box is bounded from above, . The corresponding entanglement entropy

is a periodic function of .The string inspired black hole [222, 169] is described by the metric function . It described an asymptotically-flat spacetime. The Hawking temperature is . The entanglement entropy in this case is

The entropy in these two examples resembles the entanglement entropy in flat spacetime at zero temperature (11) and at a finite temperature (12) respectively.

Living Rev. Relativity 14, (2011), 8
http://www.livingreviews.org/lrr-2011-8 |
This work is licensed under a Creative Commons License. E-mail us: |