BTZ black hole

The BTZ black hole, named after Máximo Bañados, Claudio Teitelboim, and Jorge Zanelli, is a black hole solution for (2+1)-dimensional gravity with a negative cosmological constant.

History

In 1992 Bañados, Teitelboim and Zanelli discovered the BTZ black hole solution (Bañados, Teitelboim & Zanelli 1992). At that time, it came as a surprise because it is believed that no black hole solutions are shown to exist for a negative cosmological constant and BTZ black hole has remarkably similar properties to the 3+1 dimensional black hole, which would exist in our real universe.

When the cosmological constant is zero, a vacuum solution of (2+1)-dimensional gravity is necessarily flat (the Weyl tensor vanishes in three dimensions, while the Ricci tensor vanishes due to the Einstein field equations, so the full Riemann tensor vanishes), and it can be shown that no black hole solutions with event horizons exist. By introducing dilatons, we can have black holes. We do have conical angle deficit solutions, but they don't have event horizons. It therefore came as a surprise when black hole solutions were shown to exist for a negative cosmological constant.

Properties

The similarities to the ordinary black holes in 3+1 dimensions:

It has "no hairs" (No hair theorem) and is fully characterized by ADM-mass, angular momentum and charge.
It has the same thermodynamical properties as the ordinary black holes, e.g. its entropy is captured by a law directly analogous to the Bekenstein bound in (3+1)-dimensions, essentially with the surface area replaced by the BTZ black hole's circumference.
Like the Kerr black hole, a rotating BTZ black hole contains an inner and an outer horizon (see also ergosphere).

Since (2+1)-dimensional gravity has no Newtonian limit, one might fear that the BTZ black hole is not the final state of a gravitational collapse. It was however shown, that this black hole could arise from collapsing matter and we can calculate the energy-moment tensor of BTZ as same as (3+1) black holes. (Carlip 1995) section 3 Black Holes and Gravitational Collapse.

The BTZ solution is often discussed in the realm on (2+1)-dimensional quantum gravity.

The case without charge

The metric in the absence of charge is

ds^{2}=-{\frac {(r^{2}-r_{+}^{2})(r^{2}-r_{-}^{2})}{l^{2}r^{2}}}dt^{2}+{\frac {l^{2}r^{2}dr^{2}}{(r^{2}-r_{+}^{2})(r^{2}-r_{-}^{2})}}+r^{2}\left(d\phi -{\frac {r_{+}r_{-}}{lr^{2}}}dt\right)^{2}

where $r_{+},~r_{-}$ are the black hole radii and $l$ is the radius of AdS₃ space. The mass and angular momentum of the black hole is

M={\frac {r_{+}^{2}+r_{-}^{2}}{l^{2}}},~~~~~J={\frac {2r_{+}r_{-}}{l}}

BTZ black holes without any electric charge are locally isometric to anti-de Sitter space. More precisely, it corresponds to an orbifold of the universal covering space of AdS₃.

A rotating BTZ black hole admits closed timelike curves.

References

Notes

Bibliography

Bañados, Máximo; Teitelboim, Claudio; Zanelli, Jorge (28 September 1992), "The Black hole in three-dimensional space-time", Phys. Rev. Lett., American Physical Society, 69 (13): 1849–51, arXiv:hep-th/9204099v3, doi:10.1103/PhysRevLett.69.1849
Carlip, Steven (2005), Conformal Field Theory, (2+1)-Dimensional Gravity, and the BTZ Black Hole, arXiv:gr-qc/0503022v4
Carlip, Steven (1995), The (2+1)-Dimensional Black Hole, arXiv:gr-qc/9506079
Bañados, Máximo (1999), Three-dimensional quantum geometry and black holes (PDF), arXiv:hep-th/9901148v3, doi:10.1063/1.59661
Ida, Daisuke (30 October 2000), "No Black Hole Theorem in Three-Dimensional Gravity", Phys. Rev. Lett., 85 (18): 3758–60, arXiv:gr-qc/0005129, doi:10.1103/PhysRevLett.85.3758

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BTZ black hole

History

Properties

The case without charge

See also

References