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Large D limit of Einstein’s equations

Roberto Emparan and Christopher P. Herzog
Rev. Mod. Phys. 92, 045005 – Published 18 November 2020

Abstract

Recent progress in taking the large dimension limit of Einstein’s equations is reviewed. Most of the analysis is classical and concerns situations where there is a black hole horizon, although various extensions that include quantum gravitational effects are discussed. The review consists of two main parts: the first is a discussion of general aspects of black holes and effective membrane theories in this large dimension limit, and the second is a series of applications of this limit to interesting physical problems. The first part includes a discussion of quasinormal modes that leads naturally into a description of effective hydrodynamiclike equations that describe the near-horizon geometry. There are two main approaches to these effective theories, a fully covariant approach and a partially gauge-fixed one, which are discussed in relation to each other. In the second part the applications are divided up into three main categories: the Gregory-Laflamme instability, black hole collisions and mergers, and the anti–de Sitter/conformal field theory correspondence (AdS/CFT). AdS/CFT posits an equivalence between a gravitational theory and a strongly interacting field theory, allowing the spectrum of applications to be extended to problems in hydrodynamics, condensed matter physics, and nuclear physics. The final, shorter part of the review describes further promising directions where there have been, as yet, few published research articles.

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  • Received 25 March 2020

DOI:https://doi.org/10.1103/RevModPhys.92.045005

© 2020 American Physical Society

Physics Subject Headings (PhySH)

Gravitation, Cosmology & Astrophysics

Authors & Affiliations

Roberto Emparan*

  • Departament de Física Quàntica i Astrofísica and Institut de Ciències del Cosmos, Universitat de Barcelona, Martí i Franquès 1, E-08028 Barcelona, Spain and Institució Catalana de Recerca i Estudis Avançats (ICREA), Passeig Lluís Companys 23, E-08010 Barcelona, Spain

Christopher P. Herzog

  • King’s College London, The Strand, London WC2R 2LS, England

  • *emparan@ub.edu
  • christopher.herzog@kcl.ac.uk

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Issue

Vol. 92, Iss. 4 — October - December 2020

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Images

  • Figure 1
    Figure 1

    Radial potentials Vs(r*) for perturbations of the Schwarzschild black hole for n=8 and =2. The horizon is at r*. We use the coding dotted black for tensor, dashed red for vector, and solid blue for scalar in this and the next two figures. Units are r0=1.

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  • Figure 2
    Figure 2

    Radial potentials Vs(r*) for n=997 and =2. On the right is an enlargement of the potential near the peak at r*1.

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  • Figure 3
    Figure 3

    Quasinormal modes at D1: nondecoupled modes near the peak of the potential have high frequencies and straddle between the near and far zones. Decoupled modes have low frequencies and are trapped in the near-horizon geometry.

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  • Figure 4
    Figure 4

    The profile m(r) for (a) the spinning black disk and (b) the spinning black bar. From [13].

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  • Figure 5
    Figure 5

    Phases of spinning disk large D, i.e., Myers-Perry black holes (dashed blue line) and spinning black bars (black line) in the plane (J/M,Ω). The dots indicate the presence of nonaxisymmetric corotating zero modes for the spinning disks and bars. The dots in the disk branch encircled in black indicate axisymmetric zero modes. New families of solutions branch from all of these zero modes, as explored in greater detail by [164]. From [13].

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  • Figure 6
    Figure 6

    For D<D*, there are no weakly nonuniform black strings in the region where the uniform black strings are dynamically unstable. Therefore, the latter cannot evolve into the former. The phase transition must happen at some M*>MGL and be first order. For D>D*, there do exist weakly nonuniform black strings for the dynamically unstable black strings to decay into, which is consistent with a second-order phase transition at M=MGL. From [94].

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  • Figure 7
    Figure 7

    Two spinning black holes collide and form a rotating black bar, which then breaks up into two outgoing black holes unlike the initial ones. From [7].

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  • Figure 8
    Figure 8

    Stable blobs as the end points of merger evolution [cf. Fig. 5 and 164]. Solid (dashed) lines are stable (unstable) stationary blobs. Myers-Perry black holes, stable up to J/M=2; black bars, stable up to J/M=4/32.31; black dumbbells, stable up to J/M2.66 (dumbbells along the dashed line are more like unstable binaries of blobs). No stable stationary blobs exist for J/M2.66, so if a merger occurs in this region, it can evolve only to a horizon pinch, violating cosmic censorship. From [6].

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  • Figure 9
    Figure 9

    (a) Phase diagram for the solution to the Riemann problem in a large D limit. Given a pair (mL,0) and (mR,pR), the selection of shock and rarefaction waves is determined by the value of mR/mL and pR/mL. The dashed and solid lines are critical: The dashed line indicates the values of (mR,pR) connected to (mL,0) by a single rarefaction wave, while the solid line indicates the value of (mR,pR) connected to (mL,0) by a single shock wave. (b) Snapshot of the time evolution of the energy density for a RS case. x is the rescaled position coordinate, while δm=(mLmR)/(mL+mR) and m=(mL+mR)/2. From [135].

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  • Figure 10
    Figure 10

    Black hole temperature as a function of radius for D=5. Approaching from the large black hole branch, the circle indicates the Hawking-Page phase transition to thermal or empty AdS in the canonical ensemble, the square is the point at which the heat capacity becomes negative, and the triangle is the Gregory-Laflamme-type instability ([142]). As D gets larger, the three special points approach each other. From [133].

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