Attempts at vacuum counterexamples to cosmic censorship in AdS

We consider vacuum solutions of four dimensional general relativity with $\Lambda<0$. We numerically construct stationary solutions that asymptotically approach a boundary metric with differential rotation. Smooth solutions only exist up to a critical rotation. We thus argue that increasing the differential rotation by a finite amount will cause the curvature to grow without bound. This holds for both zero and nonzero temperature, and both compact and noncompact boundaries. However, the boundary metric always develops an ergoregion before reaching the critical rotation, which probably means that the energy is unbounded from below for these counterexamples to cosmic censorship.

infinity. Although it is usually discussed in the context of four-dimensional asymptotically flat spacetimes, there has been recent interest in higher dimensions and other boundary conditions. We will stay in four-dimensions, but consider asymptotically anti-de Sitter (AdS) spacetimes. This is motivated by gauge/gravity duality which relates gravity with this boundary condition to a nongravitational gauge theory [2].
In this context, a class of counterexamples to cosmic censorship has recently been found if one adds a Maxwell field [3,4]. In asymptotically AdS spacetimes, one is free to specify a boundary (conformal) metric and boundary values of any matter fields that might be present.
If one assumes certain static profiles for the asymptotic vector potential and multiplies them by an overall amplitude a, it turns out that static, nonsingular, T = 0 solutions only exist up to a maximum amplitude a max (which depends on the profile). These are static selfgravitating electric fields which become singular as a → a max . It was then shown [4] that if one considers a time dependent boundary condition where the amplitude starts with a < a max and ends with a > a max , the electric field and hence the curvature grow as a power This is the first of two papers in which we present vacuum analogs of these counterexamples. Instead of adding a Maxwell field, we will add differential rotation to the boundary metric. In this paper we construct families of smooth stationary solutions with boundary metrics of this type. A similar setup was studied in [5], where a dipolar differential rotation was added at the conformal boundary using global coordinates. We will show that if one keeps the profile of the differential rotation fixed, but increases the overall amplitude, smooth solutions only exist up to a finite maximum amplitude a max . In part II, we will study the time dependent problem of increasing the amplitude from a < a max to a > a max .
We will find that the curvature again appears to increase without bound.
We consider both T = 0 and T > 0 solutions, and boundaries that are both compact and noncompact. In all cases the results are qualitatively the same. There is a finite amplitude, a max , beyond which smooth stationary solutions do not exist. However, before reaching a max , both the boundary metric and bulk spacetime develop an ergoregion, i.e., a region of spacetime where the time translation Killing vector becomes spacelike 1 . If a ergo denotes the amplitude at which the ergoregion first forms, we will see that a max − a ergo can be made as small as one likes by varying the profile or temperature, but it is always positive. The existence of an ergoregion raises several questions which we now address.
First, one might wonder if the energy remains bounded from below if the boundary metric has an ergoregion. The existing proofs of positive energy in AdS [6][7][8][9] are not general enough to apply directly. Perturbations in the ergoregion can lower the energy a bit, but we will argue in section V that that the energy indeed remains bounded from below. Intuitively, as you lower the energy, the ergoregion shrinks toward the boundary, where subsequent perturbations cannot change the energy by much.
Second, spacetimes with ergoregions in AdS may be unstable due to superradiant scattering. This is known to happen when the ergoregion surrounds a spherical black hole. Certain modes can scatter off the black hole and return with greater amplitude. They then reflect off infinity and scatter off the black hole repeatedly, leading to an instability. The endpoint of this instability is not known although there has been some remarkable recent numerical progress [10]. It may in fact violate weak cosmic censorship in vacuum [11,12]. In our case, the ergoregion is in the asymptotic region and it is not clear if a superradiant instability exists, since ingoing waves are partially absorbed by the horizon and return with smaller amplitude. This can compensate for the enhanced scattering off the ergoregion. We will leave open the question of whether some of our stationary solutions have a superradiant instability, but argue that even if they do, it will not affect the outcome of the time dependent problem where a(t) grows larger than a max . Furthermore, the endpoint of these new counterexamples probably represents a more serious violation of cosmic censorship than proposed before. A likely endpoint of the superradiant instability is the formation of arbitrarily small black holes. The curvature would become large in small regions near the horizon, and only a tiny amount of mass would be involved. In our examples the curvature becomes large over much larger regions of spacetime.
Even if it is present, the superradiant instability is very different from the instability that results from adding a scalar field with charge q and mass m to the electromagnetic counterexamples. In that case, it was shown that the Einstein-Maxwell solutions that violate cosmic censorship become unstable to turning on the scalar field if q/m is large enough [13]. Furthermore, once the scalar field becomes nonzero, one can no longer violate cosmic censorship. Surprisingly, the minimum value of q/m to preserve cosmic censorship turned out to be precisely that predicted by the weak gravity conjecture [14] adapted to AdS. Since our current counterexamples to cosmic censorship have a similar effect on the geometry but do not involve any electromagnetic fields, they cannot be removed by invoking the weak gravity conjecture 2 .
Our solutions with T > 0 have a standard black hole horizon in the interior. But the infrared behavior of the T = 0 solutions depends on the fall-off of the differential rotation.
If it falls-off faster than 1/r, the effects of the rotation die off as one moves into the bulk and the solution has a standard Poincaré horizon. If it falls off like 1/r, there is a new extremal horizon which we will describe explicitly. If the profile is exactly 1/r, the solution has an additional scaling symmetry and can be written analytically. We call this the "spinning top" solution since the angular momentum density is concentrated at the origin. It can be viewed as the vacuum analog of the analytic "point charge" solution found in [16].
In many cases, the boundary metrics and bulk black holes that we construct will be axisymmetric as well as stationary. This raises the possibility that there may be a nonaxisymmetric, stationary black holes with a > a max . This is not possible in asymptotically flat spacetimes, but might occur in AdS [11]. To check this, we will study some cases where the only symmetry of the boundary metric is the stationary Killing field. We again find there is a maximum amplitude for smooth solutions, so relaxing the symmetry does not remove these counterexamples to cosmic censorship.
As a by-product of our analysis, we can use gauge/gravity duality to make some comments about strongly coupled gauge theories on spacetimes with ergoregions but no horizons. We will discuss this in section V.
In the next section we briefly review how to numerically construct stationary vacuum solutions. Sections III and IV give some further details on the construction and contain our main results for stationary solutions with rotating planar (III) or compact (IV) boundary metrics. We show there is a maximum amplitude and describe some properties of the solutions. In the last section we give arguments that the energy is bounded from below, discuss some implications for the dual field theory and mention some open problems. 2 Adding fields with large spin might avoid this class of counterexamples. If so, it might be viewed as a result of a spinning version of the weak gravity conjecture [15].

II. CONSTRUCTING GENERAL ROTATING DEFECTS
We will be interested in finding stationary, asymptotically AdS solutions of Einstein's equation: where L is the AdS length scale and R ab the four-dimensional Ricci tensor associated with the metric g ab . Throughout this manuscript we work with G 4 = 1.
In order to find solutions to (II.1) numerically we will use the so called DeTurck method, which was first presented in [17] and reviewed in great detail in [18,19]. The idea is to consider the following modification of Eq (II.1) where ξ a = [Γ(g) a bc − Γ(ḡ) a bc ]g bc is the so called DeTurck vector, Γ(g) is the Levi-Civita connection associated to a metric g andḡ is a reference metric which will be related to our choice of gauge. In terms of spacetime coordinates, we have ξ a = −2x a + H a , where H a ≡ −Γ(ḡ) a bc g bc does not explicitly depend on derivatives of g. Solutions of the Einstein equation (II.1) will be solutions of the Einstein-DeTurck equation (II.2) withḡ = g, however, the converse might not always be true. That is to say, it is not clear whether solutions of (II.2) will necessarily be solutions of (II.1), i.e. solutions with ξ a = 0 might exist.
However, most of the boundary metrics we will consider are stationary, axially symmetric and have a (t, φ) → −(t, φ) reflection symmetry, all of which extend into the bulk. Under these symmetries, Figueras and Wiseman have shown in [20] that ξ must vanish on solutions of (II.2). The advantage of solving Eq. (II.2) instead of Eq. (II.1) is immense, since the former represents a system of elliptic equations which can be readily solved using a standard relaxation procedure. The gauge, which is dynamically determined during the numerical procedure, is given by ξ = 0 ⇒ 2x a = H a .

III. PLANAR SOLUTIONS
In this section we discuss stationary, axisymmetric solutions to (II.1) with boundary metrics of the form with ω(r) = a p(r).

(III.2)
These metrics describe geometries with differential rotation with an amplitude a and profile p(r). We will demand that p(r) → 0 as r → ∞.

A. Zero temperature solutions
We start by considering solutions at zero temperature. It is clear from (III.1) that ω(r) must have (mass) dimension one. So if it falls off like a/r n , the dimension of a must be 1 − n.
Thus for n > 1, turning on a represents an irrelevant deformation of the boundary metric and the solution should have a standard Poincaré horizon. We will see below that this is indeed the case. For n < 1, turning on a is a relevant deformation and the solution will be very different in the infrared. For n = 1, a is dimensionless and corresponds to a marginal deformation. In this case, the extremal horizon is deformed in a way that we now describe.

Holographic spinning top
When ω(r) = a/r everywhere, the boundary metric has a new scaling symmetry: t → λt, r → λr. In fact, the conformal metric is invariant under an SO(2, 1) × SO(2) subgroup of the full SO(3, 2) conformal group of flat space. The corresponding bulk solution also has this extended symmetry and can be described analytically. In fact, it can be obtained by a double Wick rotation of a hyperbolic Taub-Nut black hole in AdS 4 [21], which is an algebraically special solution in the Petrov classification.
The resulting solution can be written with G(η) = n 2 3n 2 − 1 η 3 + 6n 2 − 1 η 2 y 2 + + 1 + η + η 2 y 4 + , and H(η) = y 2 + + n 2 η 2 . (III.4) Here, η ∈ (0, 1] with η = 0 being the asymptotic boundary and η = 1 is the axis of rotation for ∂ φ . The first term in parenthesis on the right is AdS 2 with a horizon at ρ = 0. This null surface defines a degenerate horizon for the full four dimensional spacetime, so the solution has zero temperature. The solution depends on two parameters, y + and n, and for generic values of them, there is a conical singularity along the rotation axis η = 1. This can be readily avoided by demanding with 2 = 1. For = −1, we need to restrict y + ≤ 1/3, but this implies that G(η) would have an additional root smaller than unity. We are thus left with = 1 to avoid any conical singularities, which also means 0 < y + ≤ 1. The solution with y + = 1 has n = 0, G(η) = 1 + η, and corresponds to pure AdS 4 .
Following [22] one can compute the resulting holographic stress energy tensor analytically, and fix the conformal frame by demanding that the boundary metric has fixed g tt ∂ = −1. To accomplish this, we first change to Fefferman-Graham coordinates via the following asymptotic expansion which brings the metric into the following asymptotic form In the above expression we have and Eq. (III.9a) allows us to identify ω(r) = 2n/r for this particular profile, and thus a = 2 n, with n given by Eq. (III.5). Since 0 < y + ≤ 1, a has a maximum value at y + = 1/3 which corresponds to a max = 4/3. For a = a max , the solution exhibits no bulk curvature singularity, but we believe this is due to some special fine tuning induced by this very special profile. It is significant that a max > 1. For a = 1, ∂ t is null everywhere on the boundary and for a > 1, it is spacelike. Thus the bulk solution develops an ergoregion before reaching a max . a = 1 is reached when y + = 1/3 + √ 7/6, corresponding to n = 1/2. As y + increases from zero to one, a does not change monotonically. In Fig. 1 we plot a as a function of y + and mark both the onset of the ergoregion, a = 1, and a = a max .
The holographic stress energy tensor is given in terms of ds 2 3 by where Greek indices run over the boundary spacetime directions. It is easy to see that the angular momentum density, which is proportional to T t φ , vanishes for all r > 0, so it might at first seem that the total angular momentum will be zero. However, in deriving III.10 we have completely neglected the fact that g tφ is singular at r = 0. If we were to take that into account, III.10 would have a δ(r) contribution to the angular momentum density. Instead of keeping track of this contribution, we use the methods developed in [23] to compute the total angular momentum. It turns out to be given by: (III.11) Note that J ≥ 0 only for y + ∈ [1/3, 1] and becomes negative for smaller y + . This change in sign occurs precisely at a max . (See Fig. 2 for a plot of J as a function of a.) At present we have no understanding of why this is the case. This dependence of J on the amplitude turns out to be independent of the details of the differential rotation ω(r), and only depends on the fact that ω = a/r asymptotically. We will recover Fig. 2 (for J > 0 ) when we construct zero-temperature solutions whose profile decays at large r as 1/r, but is regular as r → 0.
In fact, the entire solution (III.3) is universal in the sense that it provides the near horizon geometry for this class of profiles.

Metric ansatz
We first discuss the metric ansatz for profiles that fall off faster than 1/r asymptotically, which correspond to irrelevant deformations of the boundary. These solutions should have standard Poincaré horizons in the IR. We will use the coordinates first described in [16] and recently used in [4,13]. We start with AdS written in Poincaré coordinates where z ∈ [0, +∞), with z = 0 marking the location of the conformal boundary, and z = +∞ the Poincaré horizon. Furthermore, (r, φ) are standard polar coordinates in R 2 , with r = 0 marking the axis of rotation. We now introduce two new coordinates (x,ỹ) which compactify both r and z in the following form 13) with (x,ỹ) ∈ [0, 1] 2 . In terms of the (t,x,ỹ, φ) coordinates, the metric on Poincaré AdS reads (III.14) The Poincaré horizon is now atỹ = 1, where the above metric reveals an AdS 2 like throat characteristic of zero temperature horizons. The boundary is located atx = 1 andỹ = 0 (ỹ = 0 just corresponds to the point z = r = 0), andx = 0 marks the axis of rotation. We note that, at the boundary, the relation betweenỹ and r, reduces to (III. 15) In order to use the DeTurck method we need to write down the most general line element compatible with our symmetries. Recall that our boundary metric has two commuting Killing fields, ∂ t and ∂ φ and an additional discrete symmetry (t, φ) → −(t, φ). We assume that these symmetries extend smoothly into the bulk. The most general line element compatible with general diffeomorphisms along the (x,ỹ) directions takes the following form 16) where q i , with i ∈ {1, . . . , 6}, are the functions of (x,ỹ) we wish to determine.
Four our reference metric we take where g(ỹ) will control our chosen boundary profile for the differential rotation.
The case of marginal deformations (ω ∼ 1/r) is different, since we expect the IR to be deformed away from pure AdS into the family of exact solutions discussed in section III A 1.
The metric ansatz remains as in Eq. III.16 except we set q 6 = (1 −ỹ 2 )q 6 , and express all boundary conditions in terms ofq 6 . Note that this means at the boundary (both atx = 1 andỹ = 0) we wantq 6 = a, and that at the symmetry axis we still have ∂xq 6 = 0. The only significant change comes at the would be Poincaré horizon, where we impose which are enforced via regularity in ingoing Eddington-Finkelstein coordinates.

Results
We will first focus on the following class of profiles for the differential rotation: where A is the boundary profile amplitude, σ is a length scale, and n is a positive integer 3 . At large r, these profiles decay like 1/r n . Since the boundary metric (III.1) is only determined up to conformal rescalings, we can always rescale A and σ such that the only meaningful quantity is a ≡ Aσ. We will fix σ = 1 in the numerics, and so A = a. In terms of theỹ coordinate (III.15), we have (III.23) We start with results for n > 1. (The special case n = 1 will be discussed shortly.) For each fixed value of n, we construct the solutions numerically by increasing a starting with for various profiles. All of these solutions have a standard Poincaré horizon as expected. For the above class of profiles, a ergo is given by For a > a ergo , the ergoregion is an annular region around the origin on the boundary, and extends into the bulk. For a = a ergo the ergoregion collapses to a single circle and has been called an evanescent ergoregion [24]. It does not extend into the bulk. Note that both a max and a ergo increase with n. So when the differential rotation on the boundary falls off faster, solutions exist for a larger amplitude. It is also clear from Fig. 3 that the difference a max − a ergo increases with n. 4 The error bars in determining a max simply reflect the fact that a solution exists at the blue dot but not at the upper end of the error bar (using a uniform grid over a). In the following, when we quote results for a max , we mean this largest value for which we have found a solution, and not literally the singular solution. To show the formation of a singularity as we approach a max , we monitor the square of the Weyl tensor C abcd C abcd throughout spacetime. Let where M denotes our spacetime manifold. In Fig. 4 we plot C max as a function of a for n = 8. The rapid growth as a → a max is clearly visible. To gain more information about where the singularity appears, in Fig (In these coordinates, the asymptotic boundary isx = 1.) Within our symmetry class, the holographic stress energy tensor has four non-zero components. In addition, it should be traceless and conserved, which gives two constraints amongst these four components. Thus, the full stress energy tensor is determined by ρ and j.
Two important questions are whether ρ and j change their behavior qualitatively after the ergoregion forms on the boundary, and whether they diverge as we approach a max . To check this, we computed the holographic stress energy tensor using [22], and following mutatis mutandis section III B 1. We find that the answer to both questions is no: the formation of the ergoregion does not dramatically affect these quantities and they appear to remain finite. This is illustrated in Fig. 6 for n = 2 and several values of a, including a = a max (most right column). Note that the scales on the vertical axis are different in the six plots, and the maximum values of |ρ| and |j| tend to increase with a. Curiously, although ρ remains finite, for a = a max it reaches a maximum precisely at the edge of the ergoregion. We see this happening for all values of n, and for different profiles. Note that even though we have imposed a differential rotation ω(r) that is positive everywhere, the induced angular momentum density j takes both positive and negative values. In fact, the total angular momentum, J, in the spacetime turns out to be exactly zero (to machine precision). This is directly analogous to what was found in [16] where static solutions of Einstein-Maxwell were discussed. There it was shown that a localized positive chemical potential that falls off The total energy is plotted in Fig. 7 for n = 8. We note that the energy is always positive even after the formation of the boundary ergoregion, denoted by the vertical dashed line i.e. a = a ergo . The behaviour of the energy as we approach a max is puzzling to us, i.e. we do not understand why it is not monotonic with increasing a.
It is clear from Fig. (3) that the difference a max − a ergo depends on the profile for the differential rotation. It turns out that one can make this difference arbitrarily small by a judicious choice of profile 5 . One way to do this is to choose a profile that is very sharply 5 We will see in section III B that another way to make this difference arbitrarily small is to go to high temperature. peaked at the origin. Consider We have added a new parameter b, which controls the height and thickness of the profile around r = 0. In terms of the coordinate (III.15), this profile reads To see the effect of b, we set a = 1 and decrease b. Then g tt = −1 + r 2 ω 2 (r) < 0 everywhere for b > 0, but vanishes at r = 0 when b = 0. So the ergoregion first forms at the origin in this case. Note that for b = 0, the profile looks like a/r near the origin, just like the spinning top solution discussed in section III A 1. We now compute the maximum curvature To see if we could find situations where a max is reached before an ergoregion exists, we considered a class of rotating boundary geometries without ergoregions: suggests that the solution stops existing precisely when an ergoregion first forms.
These solutions can be constructed exactly as before (section III A 2), except that we change our reference metric to be such that no ergoregion is present. For the reference metric we take all functions as in Eq. (III.17), except for q 1 which is now given by The form of ω(r) is again given by (III.23). We studied in great detail the cases with n = 2, 4, 6, 8 and we found no upper bound on a. In all these cases, we were able to reach a ∼ 20 without seeing any indication that the solution is becoming singular. In Fig. 9 we plot C max as a function of a for n = 2. Contrary to the case where the ergoregion is present, the maximum now occurs along the axis of rotation.
Finally, we briefly discuss the case n = 1. There are two qualitative differences from the n > 1 solutions. First, the IR geometry is not given by a standard Poincaré horizon, but rather by the extremal horizon of a member of the holographic spinning top solution discussed in section III A 1. In other words, any profile that asymptotically behaves like ω(r) ∼ a/r has the same IR geometry as the solution where ω(r) = a/r everywhere. Note that our boundary conditions (III.21) do not impose this as a Dirichlet condition. Instead, this emerges as the natural IR solution.
Second, the total angular momentum is no longer zero. Since our n = 1 boundary profile indication that the metric is becoming singular at any finite value of a. The solid red line is the result for the spinning top shown in Fig. 2.
is not singular at r = 0, we can compute the total angular momentum just by integrating the angular momentum density. The result is depicted in Fig. 10, where we also superimpose our exact result (III.11). We see that the angular momentum of the regular profile agrees with that of the spinning top with the same coefficient of the 1/r fall-off.

Stability analysis
For a < a ergo , we expect our solutions to be stable, but for a > a ergo , they may be unstable to nonaxisymmetric perturbations due to the superradiant instability. To investigate this, instead of studying the full gravitational perturbations, we will study perturbations by a massless scalar field. So we add a field Φ satisfying the massless wave equation Since the background is stationary and axisymmetric, we can Fourier decompose Φ as and find the quasinormal mode spectrum, i.e. the complex values of ω for which Φ is normalisable at the conformal boundary, and regular at the horizon. We are primarily interested in finding the onset of the instability, which occurs for ω = 0. We can then interpret Eq. (III.32) as an eigenvalue equation for m 2 for a given value of a. Of course, we want m ∈ Z, since φ is chosen to have period 2π.
We now have to discuss the thorny issue of boundary conditions. The best way to do this is to expand Eq. (III.32) around each of our integration boundaries and use Frobenius's method to extract the leading non-analytic behaviour. For ω = 0, we find the following behaviour: where p is an integer and C + is a smooth function aroundỹ = 0. In terms of the original coordinates (r, z) of the line element (III.12) this reads where C + is a smooth function of r 2 + z 2 . Regularity at the origin thus demands p = 0.
Note that the factor r |m| is needed to cancel the non-analytic behaviour of e imφ included in Eq. (III.33). We thus perform the following change of variables and solve for Φ numerically. All we are missing is a choice of boundary conditions. Atx = 0 andx = 1 we find ∂x Φ = 0, while atỹ = 0 we have ∂ỹ Φ = 0. Finally at the Poincaré horizon we find Φ = 0.
In Fig. 11 we show the results of our stability analysis. Our solutions all become unstable before we reach a max . We plot the amplitude for the onset of the instability for a variety of modes, 5 ≤ m ≤ 18, and for several profiles, 2 ≤ n ≤ 8. In all cases, the onset occurs for a > a ergo as expected. Independent of profile, the onset of the instability monotonically decreases with m, and appears to approach a ergo as m → ∞. This is similar to the results found for Kerr AdS. It supports the idea that an ergoregion is needed to have an instability, and the shortest modes become unstable first.

Scalar condensate
We now ask if there is a possible stationary endpoint for this instability. In the analogous problem involving gravity coupled to a Maxwell field, it was found that if one adds a charged scalar field, the solutions also become unstable before a max . However, it was shown that there is a stationary solution with nonzero scalar field for all amplitudes [13], so there is a natural endpoint to the instability. We now check if the same is true for our vacuum black holes coupled to a scalar field.
It turns out to be convenient to work with a complex massless scalar field so we consider the Einstein-scalar action where * denotes complex conjugation. We again use the Einstein-DeTurck equation, but including a scalar field. That is to say, we solve To ease our numerical calculations, we consider a scalar field with a definite quantum number m: with Φ being real. The matter sector breaks axisymmetry, but the metric does not since the stress energy tensor only involves Φ in the combination ∇ (a Φ∇ b) Φ * . This is similar in spirit to the black holes with a single Killing field of [25,26] and holographic Q-lattices of [27]. As before, we choose an ansatz for our scalar field of the form: Our results are rather surprising and very different from the electromagnetic case. Stationary solutions with nonzero scalar field indeed branch off from the onset of the instability.
However, they now extend towards smaller values of a. Eventually, these solutions become singular and terminate. This is depicted in Fig. 12 for n = 2 and m = 6. To judge the size of the scalar field, we use the maximum of the expectation value of the dual scalar operator over the boundary, which is essentially the coefficient of the leading term in Φ as one approaches the boundary. This is perhaps similar to the results found in [11], where the black resonators and black holes with a single Killing field of [26] extend to smaller values of the angular velocity. Since our vacuum solutions are stable for these values of the amplitude, it is likely that these new solutions with nonzero scalar field are unstable 6 . More importantly, there are no stationary configurations for the larger amplitude solutions to settle down to, even including the scalar field.

B. Black Holes
We now extend our results to nonzero temperature, to see what happens if we start with a black hole rather than the vacuum. The boundary metric will again be given by (III.1), and the differential rotation ω(r), will again take the form (III.23).

Metric ansatz
We will start by describing our choice of reference metric. First, we take the usual planar black hole written in the familiar Schwarzschild coordinates (r, Z) where the horizon is the null hypersurface Z = Z + with the associated Hawking temperature T = 3/4π Z + . According to the gauge/gravity duality, the Hawking temperature will be identified with the field theory temperature T [28].
We now introduce new coordinates in terms of which the line element (III.41) can be written as where G(y) = 3 − 3y 2 + y 4 and y + ≡ 1/Z + . In terms of these new coordinates, the profile (III.23) reduces to (III.44) We now propose the following ansatz for our metric For the reference metric we take Eq. (III.45) with q 1 = q 2 = q 3 = q 5 = 1, q 3 = 0 and q 6 = g(x).
We now discuss the issue of boundary conditions. Infinitely far away from the fixed points of ∂ φ , i.e. at x = 1, we demand q 1 = q 2 = q 3 = q 5 = 1 and q 3 = q 6 = 0, which is consistent with our choice of profile (III.44). At the centre, located at x = 0, regularity demands At the conformal boundary, located at y = 1, we choose the line element (III.45) to approach the reference metric, i.e. q 1 = q 2 = q 3 = q 5 = 1 , q 3 = 0 , and q 6 = g(x) . (III.47) Finally, at the horizon, located at y = 0, regularity in ingoing Eddington-Finkelstein coordinates imposes with the later condition fixing the black hole temperature to be Lastly, we discuss how to extract the holographic stress energy tensor, following [22].
First, we solve (II.2) in a series expansion around conformal boundary y = 1. This is done via the rather intricate expansion (III.50) The nonanalytic terms, which will affect the convergence of our numerical method, were first uncovered in [29] and [30].
Once the expansion is sorted out, the idea is to then change from our coordinates (x, y) to Fefferman-Graham coordinates via a new asymptotic expansion and determine the coefficients α i and β i by requiring the line element (III.45) to be in the Fefferman-Graham form, i.e.
where ds 2 i , with i ∈ {0, 2, 3}, only has components along the boundary directions. For instance, we find After recasting the metric is in this form, the holographic stress energy tensor is recovered via [22] T µν dx µ dx ν = 3 16 π ds 2 3 . (III.54)

Results
We have followed the same procedure as before, increasing the amplitude a for fixed temperature T , and for several different profiles: n = 2, 4, 6, 8. In all cases, we again find that there is a maximum amplitude we can attain before our solution becomes singular 7 . As a typical example, in Fig. 13 we plot the maximum value of the square of the Weyl tensor, C max (III.25) for the case n = 4 and T = .9/4π. The apparent kink in Fig. 13 results from the crossing of two local maxima, analogous to the absolute maximum going through a first order phase transition. As in the T = 0 case, a max increases with n. This is illustrated Next, we examine how a max changes when we turn up the temperature. We find that a max decreases rapidly from its T = 0 value and settles down to a ergo . To illustrate this, in Despite appearances in Fig. 15, we do not expect a max = a ergo at finite T , but only to approach it from above as T → ∞. This is because one can construct stationary black holes with large T for all a < a ergo using holography, and in particular, the fluid/gravity correspondence [31][32][33]. When the scale of curvature is much larger than the thermal wavelength, one expects the dual field theory will be well described by a fluid. In this case, the fluid/gravity correspondence constructs a bulk solution by associating a piece of a boosted planar black hole to boundary regions that are smaller than the curvature scale but larger than the thermal wavelength, and suitably patching them together. For a < a ergo one can indeed construct stationary bulk black holes using this procedure which agree very well with our numerical solutions. However one cannot obtain stationary solutions this way when there is an ergoregion on the boundary, since the Killing field becomes spacelike and can no  Fig. 16).
The total angular momentum J is now nonzero and grows with T . Unlike the total energy E, J appears to diverge as a → a max .

IV. COMPACT SOLUTIONS
In this section we consider a different class of solutions where the boundary has topology T 2 × R and we add rotation around the circles. We will mostly focus on the case where we add rotation around one circle, so the boundary metric takes the form where X and W are both periodic with periods X = 2π/k X and W = 2π/k W respectively, and ω(X) = a cos k X X .
Note that if a > 1, there is a boundary ergoregion, whereas if a < 1 there is none, so a ergo = 1.
The case a = 1 corresponds to the situation when we have an evanescent ergosurface. Unlike the non-compact case, a now always has conformal dimension 0, so it corresponds to a marginal deformation of the boundary metric.
At the end of this section, we will briefly comment on what happens if we add rotation to both circles and the boundary metric takes the form:

A. Zero-temperature solutions
We first discuss zero-temperature solutions. Even though our ansatz for the boundary metric (IV.1) has three parameters a, k X , k W , there is only a one parameter family of inequivalent solutions labelled by a. This is because we can use scale invariance to set k X = 1, and since our boundary metric is independent of W , our solution will be independent of W and W will only appear as an overall factor.
Since our boundary metrics are compact, we have a couple of possibilities for the IR behaviour of our solutions. Namely, one can have a solitonic solution, with no horizons, where a spatially compact direction smoothly caps off spacetime [34], or we can try to compactify the Poincaré horizon. If one starts with the Poincaré patch of AdS and makes the spacelike directions of the Minkowski slices compact by periodically identifying them, the horizon develops a conical singularity and is no longer smooth. This is because the translational symmetries have a fixed point there.
In a canonical ensemble, the solution that is likely to dominate at T = 0 is the solitonic one, since this is true without the rotation. However, we are interested in studying these solutions from a microcanonical perspective, since that is appropriate when evolving at fixed energy. Furthermore, we are interested in the T → 0 limit of the black holes we will construct in part B, so we will focus on the solutions with a compactified Poincaré horizon. We leave the construction of the solitonic solutions to a future endeavour.

Metric ansatz
Again, we use the DeTurck method which we outlined in section II to construct solutions.
We start with pure AdS written in familiar Fefferman-Graham coordinates where again X and W are periodic coordinates with period X ≡ 2π/k X and W ≡ 2π/k W .
We now introduce coordinates which brings Eq. (IV.5) into the following form (IV.7) The form of (IV.7) is ideal to introduce the DeTurck trick, since y = 1 marks the Poincaré horizon and y = 0 the location of the conformal boundary while the remaining two boundary coordinates have period 2π. In this section we will only study rotation profiles along the W direction, which explicitly depend on X. Our line element for the DeTurck method reads which is invariant under general reparametrizations of (x, y). For the reference metric we will take q 1 = q 2 = q 4 = q 5 = 1 , q 3 = 0 , and q 6 = a cos x . (IV.9) The boundary conditions at the IR of the theory, that is to say at the horizon located at y = 1, are simply ∂ y q 1 = ∂ y q 4 = ∂ y q 5 = 0 , q 2 = 1 and q 3 = q 6 = 0, (IV.10) while at the conformal boundary we demand our physical bulk spacetime metric to approach the reference metric (IV.9). We shall see that the IR will depend on a, but in a trivial way.
In particular, the IR will always be Poincaré, but g tt , g ww and g xx will appear renormalised along the RG flow as we move from the UV to the IR. This is to be expected, since from the perspective of the UV theory, a is a marginal deformation. The boundary conditions above are compatible with such IR behaviour. We should a posteriori check that q 1 , q 4 and q 5 are independent of x when y = 1, which will turn out to be the case for all the runs we have made.

Results
Just as in the noncompact case, there is a maximum amplitude a max beyond which the solutions develops a curvature singularity. To find a max , we again monitor the maximum value of the square of the Weyl tensor, C max , as a function of a and determine where it diverges. This is plotted in Fig. 17. Like the non-compact zero-temperature solutions of section III A 3, solutions exists even when a > a ergo = 1. In fact we find a max ≈ 1.28. We have computed other quantities such as ρ and j, but they behave just like in the non-compact case, so we will not present them here. One of the quantities of interest that we can extract from these is the energy density E/ W as a function of a. This is presented in Fig. 18, where we again see E increasing monotonically even past a = a ergo , but reaching a maximum value just before a max . Just like for the non-compact case, we have no current understanding of this behaviour.

B. Black Holes
We next discuss black hole solutions with boundary conditions (IV.1) or (IV.3). Since the temperature T is a new dimensionful parameter, inequivalent solutions can now depend on the dimensionless ratios T /k X and T /k W . Increasing the wavenumbers at fixed temperature will have the same effect as decreasing the temperature. Combined with the dimensionless amplitude a, our moduli space is thus either two or three-dimensional depending on which boundary condition we impose.

Metric ansatz
We will again use the DeTurck method. We will start by recalling the line element of a Schwarzschild black brane with toroidal spatial cross sections and we are interested in the case where both X and W are periodic with periods X ≡ 2π/k X and W ≡ 2π/k W , respectively. Next, we change to new variables in terms of which (IV.13) can be recast as where G(y) = 3 − 3 y 2 + y 4 , y + ≡ 1/Z + and x, w are periodic coordinates with period 2π.
The horizon is the null hypersurface y = 0, and has Hawking temperature (IV.14) We can now detail the ansatz we used in the DeTurck method. We recall that this ansatz should be compatible with diffeomorphism invariance in the (x, y) directions. The line element reads where all six functions q i are functions of (x, y) only. For the reference metric in the DeTurck method, we will use the line element above with The boundary conditions are determined by requiring regularity across the event horizon, which demands ∂ y q 1 = ∂ y q 2 = ∂ y q 4 = ∂ y q 5 = ∂ y q 6 = 0 , q 3 = 0 and q 1 = q 2 . (IV.17) Note that the last boundary condition ensures that the black hole temperature is given as in (IV.14). At the boundary, we give Dirichlet boundary conditions and demand the metric to approach the reference metric (IV.16) Finally, we will also briefly discuss the case where we have boundary deformations in both the x and the w directions. This corresponds to a full three dimensional problem, where the black hole has a single Killing isometry corresponding to time translations ∂/∂t. The most general line element compatible with such reduced symmetries reads where all ten functions Q i are functions of (x, y, w). For the reference metric we now choose Q 5 = a x cos w and Q 6 = a w cos x .
The boundary conditions at the horizon again following from requiring regularity across the event horizon with the later fixing the temperature to be given by (IV.14). Finally, at the conformal boundary, we demand the bulk physical metric to approach the reference metric (IV.19).

Results
We start by adding rotation around one circle. Just as in section III B we find that solutions exist only up to a maximum value a max , which strongly depends on the ratio T /k X . We first fix T /k X and increase a until the curvature, C max , appears to diverge. This is depicted in Fig. 19 for T /k X = 0.239 (top curve) and T /k X = 0.0119 (bottom curve).
In the next step, we investigate how a max depends on T /k X by repeating the same calculation that leads to Fig. 19 for many values of T /k X . The results are plotted in Fig. 20.
Again we see that a max decreases rapidly from the T = 0 result computed in the previous section to a ergo = 1 in the fluid limit (corresponding to the high-temperature regime) We also studied how ρ and j depend on T /k X at fixed a = 1.1008, which can be seen in Fig. 21 for T /k X = 0.0239, 0.0477, 0.0716. Since a > 1 there is an ergoregion on the boundary, but for these low temperatures, ρ and j change only modestly with T .
At high temperatures, the behaviour of ρ and j is dramatically different from the one depicted in Fig. 21. In Fig. 22 we show both ρ and j computed for T /k X ≈ 1.43 and a = 0.975. Although the boundary metric now does not have an ergoregion, if a is increased slightly an ergoregion forms at k X X = 0, π. Note that both the energy and momentum densities develop large features precisely at the location of the would be ergoregion. This is in perfect agreement with the fluid gravity calculation, which indicates a similar feature.
In Fig. (23) we show the analytic curve derived in the fluid approximation (represented as a dashed line) and our numerical data (represented as blue disks). The agreement even at these modest values of T /k X is very reassuring.
If we fix T /k X and increase a, the area of the event horizon increases rapidly as a → a max .
We show this behaviour in Fig. 24 where we plot the entropy density S/ W as a function of a and using T /k X ≈ 0.2387. Other values of T /k X have behave similarly.
Finally, we briefly discuss what happens if we add rotation around both circles and use boundary metric (IV.3). We will assume equal amplitude for the two rotations: a =ã. The calculations are, of course, much more time consuming since we are now solving ten coupled three-dimensional nonlinear partial differential equations. Nevertheless, we reach similar conclusions. Again we find that solutions exist up to a maximum value a max and that this can be larger than a ergo ≡ 1/ √ 2. The ergoregion now consists of disconnected disks centred at Xk X = 0, π and W k W = 0, π Perhaps the most interesting quantities to plot are now the energy density ρ and the remaining components of the stress energy tensor. These are displayed in Fig. 25 for T /k W = 0.239, k X /k W = 1, and a = 0.6. The behaviour is very similar for other values of a we have studied, except that the extrema get more noticeable as one approaches a = a max .

V. DISCUSSION
We have numerically constructed stationary, asymptotically AdS solutions of Einstein's equation with Λ < 0 with rotating boundary metrics. If we fix the profile of the differential rotation and increase the overall amplitude a, we find a maximum value a max where the solution becomes singular. This happens both at zero and nonzero temperature, and for compact or noncompact boundaries. In paper II of this series, we will study the time dependent problem where a is increased from a < a max to a > a max and show that the curvature grows without bound. Thus these spacetimes provide new counterexamples to weak cosmic censorship. The boundary metrics all develop ergoregions before reaching a max and since one can extract energy from an ergoregion, it is natural to ask if there is a positive energy theorem for these boundary conditions. Although we do not have a proof, we think it is likely that there is. Our evidence comes mainly from extensive efforts to construct initial data with negative energy. Starting with initial data taken from the stationary solution, we have modified it in various ways satisfying the constraints, and computed the total energy. We find that while the energy can be reduced below that of the stationary solution, it cannot be reduced indefinitely. This will be discussed further in paper II.
There is also an intuitive picture for why the energy should be bounded from below.
In our stationary solutions, the boundary ergoregion extends into the bulk. But as one extracts energy, the bulk ergoregion should shrink toward the boundary since one is exciting modes moving in the opposite direction to the background. Since all perturbations vanish at infinity, once the ergoregion moves sufficiently far out, the energy cannot be lowered any further. This is just an intuitive picture since once we start to lower the energy below the stationary solution, the spacetime is no longer stationary and an ergoregion cannot be defined. In particular, the minimum energy solution will not be stationary.
In light of gauge/gravity duality, our results have some implications for the dual field theory. Consider the planar case with a ergo < a < a max . The boundary metric is an asymptotically flat spacetime with an ergoregion and no horizon. Classical fields on such spacetimes are known [35] to be unstable since one can construct negative energy solutions by exciting fields in the ergoregion. Since stationary solutions must have zero energy and the energy radiated to infinity is always positive, if the energy is negative initially, it will continue to decrease. Free quantum fields on such a spacetime exhibit a similar instability: it has been shown [36,37] that there is no Fock vacuum that is time translation invariant.
In other words, there is particle creation in all states. It is also clear that there is no lower bound on the energy for free quantum fields in such a spacetime. This is because excitations localized in the ergoregion can have negative energy, and one can give them arbitrarily large occupation number.
However, we have seen that certain large N , strongly coupled field theories behave differently. The fact that stationary bulk solutions exist means that some stationary states exist.
If the bulk energy remains bounded from below as we expect, the same must be true of the field theory. This is certainly possible since interactions can make it impossible to lower the energy indefinitely by exciting many modes in the ergoregion.
Another possible source of instability in the dual field theory is negative scalar curvature.
Conformally invariant scalars in such backgrounds can be unstable. However this is not a problem for the boundary metrics we consider. In the compact case, the scalar curvature of (IV.1) or (IV.3) is nonnegative. In the noncompact case, although the scalar curvature of (III.1) can become negative, it is confined to a small area.
In the electromagnetic case, there is a family of static, T = 0 solutions for any amplitude that describe hovering black holes [16]. These are extremal spherical black holes that hover above the Poincaré horizon since the usual attraction to the horizon is balanced by an electrostatic attraction to the boundary. This family of solutions did not play any role in our counterexamples to cosmic censorship since if we only have a Maxwell field, there is no charged matter, and no way to form a charged black hole. It is natural to ask if an analogous hovering black hole could form in the vacuum case and provide a stationary endpoint for any amplitude. It appears the answer is no. We have seen that the singularity arises off the axis so it actually forms a ring. This could not be enclosed by a spherical black hole unless the black hole was quite large and unlikely to be supported by any spin-spin forces. Furthermore, the time dependent solutions that we will discuss in paper II do not show any sign of forming hovering black holes.
One open question is clearly to prove a positive energy theorem that applies to our boundary metrics. The existing proofs of positive energy in AdS [6][7][8][9] do not apply. For a < a ergo , the stationary T = 0 solutions we have constructed are presumably the minimum energy solutions with these boundary conditions. This is because we can start in the ground state at a = 0 (pure AdS) and slowly increase a. One would expect to stay in the ground state in this adiabatic process.
Another open question is to add a massive, high spin field to see if that might remove this class of counterexamples to cosmic censorship. This is motivated by the fact that the electromagnetic counterexamples to cosmic censorship can be removed by adding a massive charged scalar field satisfying the weak gravity conjecture [13].