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 topological gravity with a negative cosmological constant^{[clarification needed]}.

History

In 1992, Bañados, Teitelboim, and Zanelli discovered the BTZ black hole solution (Bañados, Teitelboim & Zanelli 1992). This came as a surprise, because 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.^[1] But thanks to the negative cosmological constant in the BTZ black hole, it is able to have remarkably similar properties to the 3+1 dimensional Schwarzschild and Kerr black hole solutions, which model real-world black holes.

Properties

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

It admits a no hair theorem, fully characterizing the solution by its ADM-mass, angular momentum and charge.
It has the same thermodynamical properties as traditional black hole solutions such as Schwarzschild or Kerr black holes, e.g. its entropy is captured by a law^[which?] 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, analogous to an ergosphere.

Since (2+1)-dimensional gravity has no Newtonian limit, one might fear^[why?] 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 AdS_3.^[2]

A rotating BTZ black hole admits closed timelike curves.^{[citation needed]}

References

Notes

^ Karakasis, Thanasis; Papantonopoulos, Eleftherios; Tang, Zi-Yu; Wang, Bin (2021). "Black holes of ( 2+1 )-dimensional f(R) gravity coupled to a scalar field". Physical Review D. 103 (6): 064063. arXiv:2101.06410. Bibcode:2021PhRvD.103f4063K. doi:10.1103/PhysRevD.103.064063. S2CID 231632352.
^ Kraus, Per (20 September 2006). "Lectures on Black Holes and the AdS3/CFT2 Correspondence". Springer Publications. 3.

Bibliography

Bañados, Máximo; Teitelboim, Claudio; Zanelli, Jorge (28 September 1992), "The Black hole in three-dimensional space-time", Phys. Rev. Lett., 69 (13): 1849–51, arXiv:hep-th/9204099v3, Bibcode:1992PhRvL..69.1849B, doi:10.1103/PhysRevLett.69.1849, PMID 10046331, S2CID 18095488
Carlip, Steven (2005), "Conformal Field Theory, (2+1)-Dimensional Gravity, and the BTZ Black Hole", Classical and Quantum Gravity, 22 (12): R85–R123, arXiv:gr-qc/0503022v4, Bibcode:2005CQGra..22R..85C, doi:10.1088/0264-9381/22/12/R01, S2CID 115762178
Carlip, Steven (1995), "The (2+1)-Dimensional Black Hole", Classical and Quantum Gravity, 12 (12): 2853–2879, arXiv:gr-qc/9506079, Bibcode:1995CQGra..12.2853C, doi:10.1088/0264-9381/12/12/005, S2CID 119508585
Bañados, Máximo (1999), "Three-dimensional quantum geometry and black holes" (PDF), Trends in Theoretical Physics II, AIP Conference Proceedings, 484: 147–169, arXiv:hep-th/9901148v3, Bibcode:1999AIPC..484..147B, doi:10.1063/1.59661, S2CID 7598959
Ida, Daisuke (30 October 2000), "No Black Hole Theorem in Three-Dimensional Gravity", Phys. Rev. Lett., 85 (18): 3758–60, arXiv:gr-qc/0005129, Bibcode:2000PhRvL..85.3758I, doi:10.1103/PhysRevLett.85.3758, PMID 11041920, S2CID 38770795

[1] Karakasis, Thanasis; Papantonopoulos, Eleftherios; Tang, Zi-Yu; Wang, Bin (2021). "Black holes of ( 2+1 )-dimensional f(R) gravity coupled to a scalar field". Physical Review D. 103 (6): 064063. arXiv:2101.06410. Bibcode:2021PhRvD.103f4063K. doi:10.1103/PhysRevD.103.064063. S2CID 231632352.

[2] Kraus, Per (20 September 2006). "Lectures on Black Holes and the AdS3/CFT2 Correspondence". Springer Publications. 3.

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