Adiabatic pumping solutions in global AdS

We construct a family of very simple stationary solutions to gravity coupled to a massless scalar field in global AdS. They involve a constantly rising source for the scalar field at the boundary and thereby we name them pumping solutions. We construct them numerically in D = 4. They are regular and, generically, have negative mass. We perform a study of linear and nonlinear stability and find both stable and unstable branches. In the latter case, solutions belonging to different sub-branches can either decay to black holes or to limiting cycles. This observation motivates the search for non-stationary exactly timeperiodic solutions which we actually construct. We clarify the role of pumping solutions in the context of quasistatic adiabatic quenches. In D = 3 the pumping solutions can be related to other previously known solutions, like magnetic or translationally-breaking backgrounds. From this we derive an analytic expression.


Introduction
Quenching a system is a way of probing its dynamics. Relevant information can be collected by studying the way the system responds and relaxes. This concerns time-dependent processes that in general have to be tackled with numerical simulations. Nevertheless, taking some specific limits allows to capture significant features without very much computational cost. Recently, the limit of fast quenches has been under intense survey allowing to extract interesting scaling relations (see [1] and references therein). In the present paper we want to study the opposite limit, where considerable simplifications occur as well: pumping solutions are very simple configurations of the Einstein-scalar theory were the real massless scalar field has a constantly increasing source at the boundary.
From the AdS/CFT perspective the pumping solutions are dual to an eternally monotonically driven conformal field theory. Actually, although being strictly speaking a time dependent setup, the metric solution is perfectly static; technically this is related to the fact that, in the massless case, the metric couples to the scalar field only derivatively. From

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the d-dimensional boundary theory viewpoint, the masslessness of the bulk scalar implies that the dual theory is monotonically deformed by means of a marginal coupling.
In this paper we will work in the context of global AdS. For the planar situation, instead, one should first cure the infrared of the theory, and some considerations in the slow quench limit have been explored in [2] using the so called hard wall model. We find agreement with them in the existence of a maximum value for the driving time slope α b and qualify this statement with some additional analysis.
The present paper is organized in five sections. In section 1 we describe the stationary pumping ansatz and the equations to be solved. We pause to clarify the difference of parameterizing the space of solutions in the origin-time or the boundary-time gauge. We describe the space of solutions and obtain their energy density. This brings us to section 2, where stability will be the main concern, both at the linear and the nonlinear level. The former study is straightforward and neat, the latter is more articulate and brings in some interesting properties like limiting cycles. Motivated by these oscillatory behaviors we search for and find time-periodic solutions, which we construct both perturbatively and numerically in section 3. These periodic solutions branch continuously from their analogs in the pure AdS geometry [3]. In section 4 we address the question of having a negative mass. We show that this effect is intimately tied to the fact that the scalar coupling rises linearly in time. Quenching back to a constant value for the scalar source restores the positivity of m. Section 5 focuses on the pumping solution over AdS 3 where, as usual, analytical control is much more attainable than in higher dimensions. In fact we provide a web of maps that links the pumping solution to a set of known models in the literature. Notably this includes magnetic horizonless and regular as well as translationally-breaking solutions. This mapping proves to be extremely useful, allowing for an exchange of explicit results from one model to the other. In particular, in this way an analytical pumping solution is obtained. We close the paper with some supplementary material linking the new solution to those encountered in seemingly very different contexts. In appendix A, we generalize the results of section 5 to higher dimensions. At the level of the equations of motion, they are shown to be derivable from a static magnetic d-form source. Appendix B, intended for the specialized reader, provides technical material containing details of the numerical construction of time-periodic pumping solutions. Finally in appendix C we discuss a possible tension of the pumping solution with respect to entanglement inequalities. We comment some caveats that need to be elucidated.

Stationary pumping solutions
Let us consider a real massless scalar field coupled to gravity plus a negative cosmological constant in d + 1 dimensions with Λ = −d(d − 1)/2l 2 . Hereafter we will set l = 1, κ 2 = d − 1 and fix the metric ansatz according to the following expression
Performing a similar expansion in d = 3 for x → π/2 and defining ρ = π 2 − x, leads to the boundary series expansion 2 In this boundary expansion, every time-dependent coefficient is a functional of φ 0 (t), φ 3 (t), δ 0 (t) and f 3 (t). In the AdS/CFT dictionary, φ 0 (t) is dual to the QFT source, while φ 3 (t) is proportional to the vev O φ . Performing a coordinate change to bring the line element (2.2) to the standard Fefferman-Graham form ds 2 = dz 2 z 2 + g ab (z,t,x) z 2 dx a dx b and expanding g ab (z, t, x) = η ab + . . . + z 3 t ab + . . . we can read off the value of the energy density m ≡ T tt = −1/2f 3 . Furthermore, the Ward identity associated to time translations reads 3 In order to look for background solutions, we plug the stationary ansatzΠ =Φ = f =δ = 0 in (2.3), and obtain the following constraints depending upon two integration constants α and β From the near origin expansion (2.6) it directly follows that β = 0, hence Φ = φ = 0 for all times. There exists a symmetry of (2.9) under δ → δ − a and α → α e a that is the JHEP05(2017)141 unbroken remnant, t → e −a t, of the group of time diffeomorphisms. Tuning a allows to select the position x p where δ(t, x p ) = 0. We consider now the boundary time gauge choice, x p = π/2, which is tantamount to setting δ 0 (t) = 0 in the near-boundary expansion (2.7). We are interested in solutions characterized by a linearly rising source φ 0 (t) = α b t where t ∈ R. In the boundary time gauge, t = t b , these sourced solutions are the natural dual to a QFT observer performing continuous quenches. α b is the pumping strength, and the label stresses the fact that its definition is linked to the boundary time gauge, where in addition one has Π(t, π/2) = α = α b .
Inserting Π and Φ = 0 into (2.4) and (2.5) we get a simple system to be solved for f and δ, namely In d = 2 these equations admit an analytic solution, while for d ≥ 3 they must be solved numerically. We will discuss the d = 3 case from now on. We consider the boundary conditions δ(π/2) = 0, f (π/2) = 1 and find that the equations can only be solved for α b ≤ α b,max . In this sense, α b,max corresponds to an intrinsic adiabaticity threshold present in our system. Here the concept of adiabaticity threshold refers to the fact that the source should grow slowly enough (with respect to the scale set by the AdS radius, α −1 b > π) in order for the system to be able to keep up with it. Solutions with faster growth are either non-regular or non-static, typically collapsing into a black hole. In the following sections we further study this key point.
Actually, the story is slightly subtler. It turns out that α b is not a faithful parameter. Instead, it will be convenient to shift momentarily to the origin time gauge choice, where the time coordinate coincides with the proper time at the origin, t = t o . The equations look exactly the same as (2.10) and (2.11) replacing δ b → δ o and α b → α o . The boundary condition to solve them now involves instead δ o (x = 0) = 0. It is clear that, in this gauge α o = Π(x = 0). Remarkably, it turns out that, for any value of α o ∈ [0, ∞) there exists a stationary solution with vanishing O φ and constantly rising scalar field figure 1 we plot a family of solutions for regularly spaced values of α 0 ∈ [0, 20]. The tension between the two parameterizations is resolved because the mapping α o → α b (α o ) is not everywhere one-to-one. Actually, it has a maximum at (α o,thr , α b,max ) = (2.01, 0.785). This can be clearly seen in the left plot of figure 2.
Let us pause here an discuss why the existence of the pumping solutions is remarkable. On general grounds, the pumping source φ 0 (t) = αt is expected to be associated with a process of energy injection that leads to a time-dependent geometry that eventually may collapse gravitationally. However, the Ward identity (2.8) readily implies that, if the pumping source is accompanied by a vanishing vev, O φ (t) = 0, the energy density remains constant,ṁ(t) = 0. This is precisely the situation in the pumping solution, since Φ(t, x) = 0. Notice that the physical mechanism behind the existence of the pumping solutions could also be the reason of its physical irrelevance: the question of whether the JHEP05(2017)141  pumping solution background is infinitely fine-tuned, in the sense that it is destroyed by any infinitesimal perturbation such that Φ(t, x) = 0, needs to be explicitly addressed.
In fact, we can compute the energy density of the pumping solutions, and perform two important observations (see figure 2, left). The first one is that there exist a threshold value α o,1 such that, for α o < α o,1 , m is negative. Similarly to other gravitational backgrounds with negative mass, this raises a concern regarding stability [4]. The second one is that there exists yet another threshold value α o,2 > α o,1 where the energy density curve m(α 0 ) reaches an extremum. We may naively think that α o,2 implies the appearance of a Chandrasekhar instability. Both issues will be discussed in the next section.
The identification of f 3 with the energy density m relies as usual on a holographic renormalization program, including finite counter-terms. Although the full holographic renormalization of the time-dependent model is beyond the scope of the present analysis, we have checked that this identification is not affected in the present setup. Indeed, despite the breaking of time translations by the background, the counter-terms must be invariant

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combinations of the induced fields on the boundary cutoff surface. Their invariance is referred to the transverse diffeomorphisms. The only new counter-term which could affect the renormalized on-shell action linear in the fluctuations (i.e. that could affect the definition of the energy density and the 1-point Ward identities) is proportional to √ −γ(∂ µ φ)(∂ µ φ), where γ is the induced metric on the boundary. Nevertheless, relying on the structure of the asymptotic near-boundary expansions of the fields, it is possible to show that such counter-term does not contribute at the finite level. 4 3 Linear and nonlinear stability of the pumping solution In order to connect two infinitesimally close pumping solutions through a normalizable fluctuation, one needs α b (α o ) = 0. Notice that this occurs at α o = α o,thr and not at α o = α 0,2 (where instead it is the mass which attains its maximal value). We recall that α b,max corresponds to α o,thr . For linearized fluctuations around the pumping solution contained in our original ansatz, an explicit computation shows that, indeed, at α b = α b,max , a zero mode appears in the eigenfrequency spectrum (see figure 2, right). Therefore, pumping solutions with α o > α o,thr are linearly unstable. This entails that, in principle, only pumping solutions with α o ≤ α o,thr can be prepared by a quasistatic quench starting from the AdS 4 vacuum.
Two questions naturally arise at this point. The first one is whether the linear stability of the α o ≤ α o,max pumping solutions translates into nonlinear stability. The second one concerns the final state reached by the α o > α o,thr pumping solutions once perturbed.
Let us address the first question. Notice first that, by virtue of the Ward identity (2.8), even if a linear eigenmode has a nonzero O φ (t) , since its time dependence is harmonic, the energy density it generates would also oscillate periodically with a π/2 phase shift with respect to O φ (t) . Nonlinear perturbations, being generically nonharmonic, might trigger a nonlinear instability due to the existence of a finite Φ(t, x) with generic time dependence, that can lead to an energy exchange eventually resulting in a gravitational collapse. There exist two complementary ways of establishing the absence of potential nonlinear instability. The first one is realizing that pumping solutions below α o,thr can be actually accessed through a quasistatic quench. Indeed, we have simulated the timedependent geometry generated by a source φ 0 (t) such that φ 0 (t < 0) = 0,φ 0 /φ 0 2 1 and lim t→∞ φ 0 /t = α b , and have checked that, at sufficiently late times, it settles down into the linearly stable pumping solution corresponding to α b (see figure 8 in section 5). In consequence, the pumping solutions play an important role at the nonlinear level: were they subjected to nonlinear instability, the system would never relax to them.
The second approach we followed in order to determine whether linearly stable pumping solutions are also nonlinearly stable was to take, as initial data at t = 0,  and simulate their subsequent time evolution. Π αo (x) represents a pumping solution characterized by α o . An example is depicted in figure 3, for α o = 1, = 1 and σ = 0.1. Due to the Gaussian perturbation, the initially negative m(0) does not remain constant: its time derivative perfectly satisfies the Ward identity (2.8) in the presence of the nontrivial O φ that is generated. Both quantities, m(t) and O φ (t) , are found to oscillate in a disordered way around their respective initial values. In fact, we find that the time-averaged energy density, m = t −1 t 0 m(t )dt , rapidly reaches a constant value and the system absorbs/loses no net energy density. Therefore, no sign of nonlinear instability is found.

The linearly unstable branch
This situation changes dramatically for the linearly unstable branch of pumping solutions. In fact, repeating the procedure described above for finite , a black hole promptly forms. Instead, initializing the simulation code with = 0, puts us exactly on top of a α o > α o,thr pumping solution, up to numerical error. Being linearly unstable, this unavoidable numerical error drives the system away from the original geometry. However, for α o,thr < α o ≤ α o,c , despite entering a time-dependent regime, the system does not undergo gravitational collapse. It rather decays into a limiting cycle that, for 0 < α o − α o,thr 1, is manifestly time-periodic. 5 Let us perform two different checks that help establishing that the limiting cycle solutions are not a numerical artifact. First, since the departure from the original unstable pumping solution is noise-driven, the transient time needed to reach the limiting cycle solution should be proportional to the grid resolution. We find that this is precisely what happens (see figure 4).
As a second check, we wait until the system has decayed into the limiting cycle solution, and take the Φ(t ref ,  The coloring encodes the three spatial resolutions N = 2 10 , 2 11 , 2 12 employed to build the initial data and perform the simulation. Consistently, the transition to a time-dependent solution happens at later times for increasing N . On the contrary, the periodicity is resolution-independent. This means that the system reaches the same limiting cycle at different times depending on the initial conditions. is implemented. Then, we perform a scan in , with the aim of seeing if the perturbed limiting cycle solution collapses gravitationally. The results of this analysis for the unstable pumping solution with α b = 0.78497 can be found in figure 5. The collapse time t c ( ) looks divergent at a critical c and, for ≤ c , no black hole forms within the times computationally accessed.

Time-periodic pumping solutions
The endpoint of the unstable pumping branch for α o < α o,c is, as said before, a limiting cycle. For 0 < α o − α o,thr 1 this limiting cycle has a single period. This fact came

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as unexpected, and prompted us to look for exactly periodic solutions with a pumping source. Time-periodic solutions in global AdS supported by a real massless scalar field with zero source were originally presented in [3] and we now show that, for α b = 0, 6 each such solution generalizes into a family of exactly periodic pumping solutions. The existence of pumping time-periodic solutions can be first proved at the perturbative level and later corroborated with a numerical approach.
Let Ω be the frequency of the periodic solution we aim at. 7 Rescale the time coordinate as τ ≡ Ω t and introduce the following ansatz At first order in α b and we are just considering the linear superposition of the pumping solution φ α (t, x) = α b t and the fundamental eigenmode of the scalar field φ = sin τ cos 3 x over global AdS 4 . Higher order corrections determine how the seed φ α + φ is dressed nonlinearly. The interested reader can find a thorough discussion with technical details in appendix B. For our present purposes it suffices to mention that, after the first nonlinear correction, the seed frequency Ω 0 = 3 is modified to To close the gap between the perturbative and the fully nonlinear regime, one needs to resort to numerical methods. In particular, since the eigenmodes of the AdS 4 Laplacian do not satisfy the boundary conditions (2.7), 8 we have adapted the pseudospectral method described in [8] to our present setup. Let us perform two different checks on the periodic solutions found numerically. We define λ as the value of the vev at τ = π/2, λ ≡ O φ (τ = π/2) = 3 . In figure 6, we plot Ω(α b , λ) for two orthogonal directions in the phase space of exactly periodic solutions, and compare it with (4.4). In each case, excellent agreement is found between the perturbative and the numerical result in the α b , 1 regime. As a further consistency check, we perform a simulation starting from Π(t = 0, x) = Π 0 (x) and Φ(t = 0, x) = 0 as determined by the pseudospectral algorithm and study their subsequent time evolution. We provide one example in figure 7. It is observed that the 6 For small αo we can equally use α b as deformation parameter since the relation that links them is one-to-one. 7 Recall that scalar eigenmodes in global AdS have a frequency spectrum given by ωn = ∆ + 2n, where ∆ is the conformal dimension of the dual scalar operator. For a massless scalar field in AdS4, ∆ = 3.  time development of the initial data perfectly agrees with the output of the pseudospectral code, providing a highly nontrivial check of our numerical procedures.

Slow and fast quenches
We have already mentioned that all pumping states with α b ≤ α b,max can be prepared by a boundary quasistatic quench α b (t). Notice that the stability analysis in section 3 was restricted to isotropic perturbations. We have seen that the fact that the pumping solution has energy density below that of AdS is not associated to an instability for small values of α o . A nice consequence of this is the fact that the pumping solution with negative mass can be obtained by means of a quench that starts from the AdS vacuum, α b = 0, and ramps this slope quasistatically to some 0 < α b < α b,max . This can be observed in the first part of figure 8, where the pumping solution is the mid part (100 < t < 300). This experimental way of building the pumping solution illustrates also the meaning of the adiabadicity threshold. Indeed, ramping α b beyond the value α b,max = 0.783 leads immediately to sudden black hole formation. In other words, there is no way to explore the region beyond α b,max by means of an experimental quench. We also want to remind the reader that all JHEP05(2017)141 Turning back to the issue of the possible puzzle with having a stable static solution with negative mass, a numerical experiment is at the same time clarifying and intriguing. Starting from a pumping solution with negative mass, like the one in figure 8 at intermediate times (100 < t < 300), we can think of suddenly isolating the system from the environment by switching off the scalar source. Naively, from the Ward identity, no energy inflow can occur and one would think that, in this way, we end up with a regular stationary solution of negative mass. However, this does not happen. Turning off the pumping can be achieved by stopping the linear growth of φ 0 as some time t f . In practice, this has to be implemented through a smooth interpolation of time span δ between the pumping boundary conditioṅ φ 0 (t < t f − δ/2) = α b and a constant final valueφ 0 (t > t f + δ/2) = 0 in the limit δ → 0. The remarkable result is that, for any value of δ and any interpolation used, the solution always returns to a positive energy density m > 0 at times t > t f + δ. In fact, for an extremely wide and smooth interpolation, the final configuration attained is the static AdS 4 background with m = 0.
For more abrupt interpolations the eventual geometry is time-dependent with a constant positive mass m > 0. An example for δ = 0.1 can be seen in figure 8. At late times, the final fate of this evolution encounters the issue of stability of a scalar pulse evolving in global AdS 4 . In fact, if we consider the limit δ → 0, the energy density peaks so violently that a direct collapse may occur immediately after t f .  interpolating functioṅ confirming that both diverge in the δ → 0 limit. A natural question is if the observed scaling is related to the fact that we are quenching off the pumping solution, or is rather determined by the particular form of the interpolating function (5.1). To answer this question, in figure 10 we plot m(δ) and max t∈[0,δ] O φ (t) for a quench with φ 0 (t) given by the time-reversed version of (5.1) acting over the AdS 4 vacuum, We observe that the former scaling relations m(δ) showing that the scaling is solely determined by the precise non-analytic behavior of the source in the δ → 0 limit: both (5.1) and (5.2) result in quench profiles φ 0 (t) that are continuous but non-differentiable. The scaling displayed by m(δ) and max t∈[0,δ] O φ (t) under (5.2) differs from the one that would be present if the quenching profile (5.2) were considered on φ 0 (t), rather than onφ 0 (t). In the case of a φ 0 (t) fast quench, the scaling relations are m(δ) ∝ δ −3 and max t∈[0,δ] O φ (t) ∝ δ −3 , as expected on purely dimensional grounds [9]. We plot representative results of this behavior in figure 11.
These numerical experiments confirm that no negative mass will be measured by a boundary observer when the source has settled to a constant value. It rises therefore the question about the nature of the quantum state dual to the pumping geometry. Is it really a bona fide quantum state? We will see in appendix C that further information coming from entropy inequalities may cast some further shadows on this.
As a further observation, note that the whole process of quenching in and off embodies some irreversible character. Imagine slowly building up the value of α b (t) from zero to a JHEP05(2017)141   In this section we shall investigate the three dimensional case. It turns out that the pumping solution over AdS 3 is related to a number of other solutions known in the literature via a series of mappings that includes double Wick rotations and/or Hodge dualities. This observation allows us to give an analytic expression for the pumping solution.
Let us consider a three-dimensional charged black brane with negative cosmological JHEP05(2017)141 constant [10,11]. The metric and the electromagnetic potential are given by In the expressions above, r ∈ [0, ∞) and t, x ∈ R. M and Q e determine respectively the mass and the electric charge of the black brane geometry. From now on, we focus on the one-parameter family of charged black branes with M = 1 and µ = 0. Note that the outer horizon is located at r = r h = 1 for |Q e | < √ 2. The temperature is At |Q e | = √ 2 the black brane is extremal. For |Q e | > √ 2, the hypersurface r = 1 actually corresponds to the inner horizon, and (6.4) does not represent the real temperature of the back brane. By performing the coordinate change r 2 = 1 + R 2 , the exterior region of the charged black brane can be parameterized as with R ∈ [0, ∞). Now, let us perform the double Wick rotation defined by in a such a way that the geometry and electromagnetic potential of the exterior region are mapped to the following solution of three-dimensional Einstein-Maxwell theory with a negative cosmological constant 10) This is a horizonless geometry. It can be explicitly shown that the coordinate ϕ must be identified with period β = 2π/(1 + Q 2 m /2) in order to avoid a conical singularity at R = 0. On the other hand, this period is nothing but the analytic continuation of the inverse temperature of the original charged black brane under the double Wick rotation.

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The geometry (6.9), (6.10) is supported by the radial magnetic field associated to (6.11), and we will refer to it as the magnetic AdS 3 solution. 9 We want to map the magnetic solution to the pumping solution. To this purpose we will rely on Hodge duality. However we have still to massage the magnetic solution: let us rescale our coordinates as t → β/(2π)t, R → 2π/βR and ϕ → β/(2π)ϕ, in such a way that ϕ ∼ ϕ + 2π. 10 In this new coordinate system, we have that

13)
where we have defined The field strength corresponding to the magnetic solution is Under Hodge duality, the magnetic AdS 3 solution can be put into correspondence with the three-dimensional pumping solution. Recall that the vacuum Maxwell equations are dF = d( F ) = 0, where is the Hodge operator. In three dimensions, the Hodge dual of a two-form corresponds to a one-form. Hence F can be alternatively expressed as F = dφ, where φ is a massless scalar field. The Bianchi identity dF = 0 transforms into the scalar field equation of motion, − d( dφ) = ∇ 2 φ = 0, while the dynamical Maxwell equation reduces to the trivial statement d 2 φ = 0. The map leaves the metric invariant and, as a consequence, a metric supported by a given electromagnetic field can be thought of as being sourced by the dual scalar field defined by this procedure.
Let us consider explicitly how the Hodge duality works at the level of the solution. Take the three-dimensional pumping solution with φ(t, r) = αt. Under Hodge duality, we find that the scalar field profile maps to 9 This background was originally found in references [12][13][14]. In [14], the authors introduced the double Wick rotation we discussed here. See [15,16] for the construction of the general magnetic solution with angular momentum, the computation of its conserved charges and a proposed physical interpretation. The physical nature of the magnetic solution was further elucidated in [17]. 10 The rescaling of the t and R coordinates follows from the requirement that limR→∞ R −2 ds 2 = −dt 2 + dϕ 2 . This corresponds to the standard flat space metric as the representative of the conformal structure of the boundary where we have chosen Ω(R) = R −2 as conformal factor. Note also that this is the same procedure we would have employed were we on the vacuum state.

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where we have parameterized the pumping solution geometry in standard Schwarzschild coordinates, Note that the radial coordinates of the magnetic AdS 3 solution and the pumping solution are related by as it emerges from comparing the ϕϕ-component of the metric (6.9) and (6.18). From a comparison of the radial components of (6.9) and (6.18), we have that r and R must also satisfy . (6.20) Deriving (6.19) and substituting into the expression above, we obtain the relation where the explicit form of h(R) provided by equation (6.13) has been employed. Note that, when R = 0, (6.13) implies that r = h(0) = 0. As a consequence, from (6.21) and the definitions of β andQ m , it follows that f (0) = 1, a fact that shows the absence of a conical singularity at the origin in a manifest way. By identifying now the tt-components of the metrics (6.9) and (6.18), we get that From (6.26), we have that the reality of Q m implies that |α| is restricted to the domain |α| ∈ 0, 1 √ 2 . Furthermore, a given α has two associated Q m parameters, Q ± , in a selfexplaining notation. The Q + branch is restricted to the domain |Q + | ∈ [ √ 2, ∞), with limits respectively attained at |α| = 1/ √ 2, α = 0. The Q − branch satisfies |Q − | ∈ [0, √ 2], and its limits correspond to α = 0, |α| = 1/ √ 2. We observe that both branches merge at the critical value |α| = α * ≡ 1/ √ 2. The two-branch structure of (6.26) is particularly interesting. Indeed, as we will show in the next subsection through an explicit computation, the Q − branch of magnetic solutions corresponds to the branch of linearly stable pumping solutions, while the Q + branch maps onto the linearly unstable branch (see section 3). Remembering how the magnetic solution has been obtained performing the double Wick rotation (6.8) on the three-dimensional charged black brane solution (6.1), (6.2), (6.3), we bring into attention that |Q e | = |Q m |. Therefore, for |Q m | = |Q + | ≥ √ 2, the linear instability of this branch of pumping solutions seems to be related to the fact that our original r 2 = 1 + R 2 expansion is performed with respect to the wrong horizon (see comments below (6.4)). In the next section we also show that α * , i.e. the critical value where the two branches of (6.26) merge, corresponds to α b,max . 11 This is an important and exact result emerging directly from the chain of mappings illustrated above. 12 The different maps we have uncovered so far are not the end of the story. Another interesting geometry can be brought into the game. In [18], Andrade and Withers (AW) introduced a beautifully simple holographic model of momentum relaxation. It involved charged black branes with nontrivial axion profiles along the spacelike boundary directions, that broke translational invariance at the level of the solution as a whole, but keeping the metric and the electromagnetic field translationally invariant. In three dimensions, the corresponding AW solution would involve a neutral massless scalar field φ(x) = γx. Focusing on the uncharged case, the metric of the AW solution would be given by By Hodge duality, the scalar field is associated with the field strength that comes from the potential A = −γ log(r)dt. If we identify γ = Q e , we find that the charged black brane and the neutral three-dimensional AW solution are dual to each

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other. Of course, we must take M = 1 after the duality map to land on the one-parameter family of charged black branes (6.1), (6.2) and (6.3). It is also possible to show that, by performing again the coordinate change r 2 = 1 + R 2 on the M = 1 AW solution, double Wick rotating as x → it, t → iϕ, γ → −iγ and rescaling our coordinates, the pumping solution is obtained. Let us summarize the structure of duality mappings through the following diagram, 13 where DW stands for the double Wick rotation.

Analytic pumping solution in AdS 3
As already anticipated before in section 6, we can employ the relation (6.19) to obtain an analytic expression for the three-dimensional pumping solution. Let us set R = R(r), identifyQ m = α and recall that β(α) = 2π/(1 + Q 2 ± /2) = π(1 ∓ √ 1 − 2α 2 ). It turns out that (6.19) can be explicitly solved, yielding where W is the Lambert W -function, which solves the transcendental equation we consistently find that R(r) 2 ≥ 0, with equality only at r = 0, a fact that is guaranteed by W (xe x ) = x. By taking (6.31) and substituting it in (6.21) and (6.23), we obtain the three-dimensional pumping solution in a closed form. It can be straightforwardly checked that the resulting expressions for f (r) and δ(r) solve the equations of motion of the pumping solution in Schwarzschild coordinates. Alternatively, if we take the relations (6.21) and (6.23) and introduce them into the equations of motion for the pumping solution with R = R(r) unknown, we arrive to the equation = 0, (6.32) for which (6.31) is the only solution such that R(r = 0) = 0. As a final consistency check, let us note that equation (6.23) implies that In figure 12, we plot δ(0) against α, 14 as obtained from the numerical solution of the equations of motion, and compare it with the expression (6.33). We plot both the stable and 13 We emphasize that the duality map between the electrically charged black hole and the magnetic solution has already been discussed in [14]. 14 Recall that α = α b , since the map between the magnetic and the pumping solutions has been obtained in the boundary time gauge.

Conclusions and future prospect
Quasistatic adiabatic quenching procedures that interpolate between two different constant values for the external source can be modeled -for a long time interval-by a coupling constant that rises linearly with a fixed slope. In the case of a marginal deformation dual to a bulk massless scalar, the physics is in the meanwhile described by the pumping solution. We have explored the space of such solutions unravelling an interesting structure of stable and unstable branches. The pumping solutions are parametrized by the slope of the ramp α which can be expressed in either the boundary time gauge, α b , or the time gauge at the bulk center, α o . There is a range of α o where the mass is negative, and this encompasses both stable and unstable solutions. Only the stable branch is reachable by a physical quench from zero coupling and zero initial slope α b (0) = 0. If one considers a ramp with a slope α b (t) > α b,max , the system destabilizes and forms a black hole. This sets a limit to the physical adiabadicity. The breaking of adiabaticity is a known phenomenon in the vicinity of a critical phase transition [1]. It is intriguing to interpret the above limit as the presence of some quantum critical point that is crossed by the protocol. Regarding this fact, note that we have not analyzed the formation time t c of the resulting black hole once the adiabaticity threshold is surpassed. It would be interesting to elucidate if t c displays some universal scaling with respect to the deviation from the threshold α b,max .
Beyond the threshold value α o ≥ α o,thr (where α o,thr corresponds to α b,max upon changing time gauge), linearized fluctuations become unstable. This is consistent with the fact that these solutions cannot be prepared through a quasistatic quench, but only exist as driving solutions that extend to t → −∞. The nonlinear analysis, however, unravels that for α o ∈ (α o,thr , α o,c ) the final fate of these unstable solutions is a limiting cycle rather than a black hole. Unfortunately, we have not been able to provide an alternative construction of JHEP05(2017)141 the limiting cycle solutions, that would definitely establish their existence on firm grounds. This is another mandatory direction for future studies.
Among the numerous future extensions, one technical but interesting direction is the proper systematization of the holographic renormalization for this time-dependent circumstance. Another future direction sprouts from the observation that the model at hand is a special example of a wider class. Indeed one could consider complex, instead of real, massless bulk fields. The complex massless scalar fields still correspond to marginal deformations, but they allow for many intriguing features such as a non-trivial scalar radial profile and a natural connection to periodically driven systems. They also provide an intermediate step to study relevant deformations in a similar setup.
We emphasize that the pumping solutions are driven setups and are not dual to vacuum configurations of the CFT. The Ward identity (2.8) and the vanishing of O φ imply however that there is no exchange of energy through the non-trivial source. It would be thereby interesting to consider the relation of the pumping solutions with models of AdS cosmology.
Regarding the three-dimensional chain of maps presented in section 6, for the moment we prefer to view it as a purely formal construction. The question of whether this construction can lead to some useful and nontrivial physical insight is definitely interesting on its own right and will be discussed elsewhere.

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the metric ansatz (2.2) as follows ds 2 = −f (r)e −2δ(r) dt 2 + f (r) −1 dr 2 + r 2 dθ + r 2 sin 2 θdϕ 2 . (A.1) On top of this, let us switch a magnetic 2-form potential B rϕ (r, θ) = 3r 2 cos θV (r) . The field strength 3-form F = dB only has one non-vanishing component From the Maxwell equations ∂ α ( √ −gF αµν ) = 0 we get the following equation for V (r) The energy momentum tensor is diagonal and with it we may compute the Einstein equations that lead to the following set If we compare these equations to the ones for the adiabatic pumping ansatz φ(t) = αt we can see that they are the same under the replacement which, by the way, solves the Maxwell's equations (A.3).

B Constructing time-periodic pumping solutions
In this appendix we provide a detailed discussion of the construction of the exactly periodic solutions described in section 4.
When solving any one of the nontrivial equations above, the requirement that ϕ 3−k,k is both regular at x = 0 and unsourced can only be satisfied if the frequency correction appearing in S 3−k,k takes a particular value. We have that ω 2,0 = −7/4, ω 1,1 = 0 and ω 0,2 = −135/128. The most general solutions compatible with the boundary conditions that we find are:  We observe that regularity and normalizability by themselves are not enough to fix the undetermined constants C 1,2 , C 2,1 , C 0,3 , D 0,3 . Notice also that, up to this point, remains as a formal expansion parameter. By ascribing a physical meaning to it we can reduce the four undetermined integration constants to one. Let us choose the definition we employed in the main text and identify O φ (τ = π/2) = 3 .

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The introduction of a finite pumping has nontrivial consequences regarding the Fourier decomposition of the exactly periodic solution in time. To wit, while in the α b = 0 case only odd multiples of the oscillation frequency Ω appear, for α b = 0 even multiples are also present, as exemplified by the ϕ 1,2 correction. It is mandatory to take this fact into account when designing a pseudospectral code able to find these solutions at the numerical level.

B.2 Numerical construction
We start by decomposing our dynamical fields as in such a way thatΠ,Φ satisfy the boundary conditionsΠ(τ, π/2) =Φ(τ, π/2) = 0 with non-zero first-order spatial derivatives. The equations of motion are correspondingly modified. Taking into account the appearance of both odd and even multiples of the fundamental frequency at the perturbative level, we Fourier decompose our rescaled fields in time aŝ where we have allowed for a nontrivial zero-mode P 0 (x) inΠ; that would take care of the fact that, when = 0, Π must reduce to field corresponding to the pumping solution at the given α b . N k is a numerical cutoff in the total mode number. The functions {P k , Q k , k = 0 . . . N k } must be further decomposed into a convenient spatial basis. A suitable choice was provided in [19] and exploited in-depth in [8] in the spherically symmetric and sourceless case. For completeness, let us elaborate a bit on this choice. We largely follow [8], and we refer the reader to that useful reference for further information.

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Therefore, for functions of well-defined parity around x = 0, if we restrict ourselves to the original spatial domain x ∈ [0, π/2] but employ the rescaled collocation grid and discretize derivatives with the just defined operator D (n) p , the desirable features of working with a Chebyshev spectral decomposition are kept while also the boundary conditions at x = 0 are automatically incorporated into the discretized problem.
Having clarified our strategy, we take the final ansatẑ so we work in mode space in τ , but real space in x. As a collocation grid in the time domain, we choose At each τ k , it is convenient to define the variables {δ k,j , c k,j }, where δ k,j = δ(τ k , x j ) and c k,j = f (τ k , x j ) exp(−δ(τ k , x j )), which are then expressed in terms of {p k,j , q k,j } by discretizing the corresponding constraint equations and inverting the resulting discretized differential operators. Imposing the boundary conditions δ k,0 = 0 and c k,0 = 1 ensures that we are working in the boundary time gauge and renders the above mentioned discretized differential operators invertible. Once this expressions are known, the first-order dynamical equations for the scalar field can be solved by means of a Newton-Raphson algorithm that we implement in Mathematica. We impose the boundary conditions p k,0 = q k,0 = 0, that follow from the linear independence of the Fourier modes of the time decomposition and Π(τ, π/2) =Φ(τ, π/2) = 0. As a last comment, notice that we have 2(N k + 1) × (N j + 1) + 1 dynamical variables, that correspond to {p k,j , q k,j } and the oscillation frequency Ω, but the discretization of the equations of motion forΠ,Φ on the two-dimensional collocation grid provides just 2(N k + 1) × (N j + 1) equations. The remaining equation comes from normalizing some relevant physical quantity to a prescribed numerical value. We choose to set where λ is an user-defined value for the vev amplitude. Since we have defined O φ (τ ) = −1/2φ (τ, π/2) =Φ (τ, π/2), this extra boundary condition is discretized as  Finally, a given family of time-periodic solutions is found iteratively: we place ourselves at λ, α b 1 and employ the perturbative solution as an initial seed to start the relaxation algorithm. Then, we move in discrete steps along the (α b (η), λ(η)) curve in the twodimensional phase space of time-periodic solutions, taking the one found in the previous step as the initial guess for the next step. The results shown in the main text of the paper have been obtained for an N k = N j = 20 grid; the time it took to find each solution along the curve was O(5) min.

C The relative entropy and the adiabatic quench
Consider two density matrix operators, ρ and σ, that describe two states of a quantummechanical system with Hilbert space H. Their relative entropy provides a measure of their distinguishability. In particular, S(ρ||σ) ≥ 0 by construction, where equality holds only for ρ = σ. We shall refer to σ as the reference state. Given that σ is Hermitean and positive definite, it can be expressed as where the Hermitean operator H σ is known as the modular Hamiltonian. In terms of H σ , the relative entropy reads where ∆ H σ = H σ ρ − H σ σ and ∆S = S ρ − S σ , with S being the von Neumann entropy of the associated density matrix (see for example [20] for an extensive review with references). For a generic σ, the modular Hamiltonian is a nonlocal operator whose explicit form is not known. The situation changes only in a handful of cases, where the modular flow associated to H σ , generated by the unitary operator U σ (s) = e −isHσ , admits a geometric interpretation. Consider a CFT placed on the Einstein Static Universe ESU d+1 = R × S d , and take the cap-like region C = {t = t 0 , θ < θ 0 : x ∈ ESU d+1 }. Let the theory be in its vacuum state |0 , and consider the reduced density matrix ρ C , which encodes any observation restricted to the causal development of C, C ≡ D(C). This reduced density matrix is obtained after partial trace over the complementary of C, ρ C ≡ trC |0 0|. The modular Hamiltonian H C ≡ − log ρ C is, in this case, a local operator given by whereT µν is the CFT energy-momentum tensor operator. Recalling (C.3), we observe that the AdS/CFT correspondence allows for an explicit computation of S(ρ||σ) if we take ρ C as reference state. Consider a fixed CFT, and a generic JHEP05(2017)141 state ρ with a dual geometric description. The GKPW prescription and the holographic renormalization procedure allow us to compute ∆ H C = 2π θ<θ 0 cos θ − cos θ 0 sin θ 0 T 00 ρ − T 00 vac . (C.5) The CFT vacuum state is now described geometrically by global AdS d+1 . On the other hand, the holographic entanglement entropy (HEE) prescription provides a way of computing the difference of von Neumann entropies ∆S, since now S ρ − S vac is nothing but the area of an extremal surface homologous to C regularized with respect to the vacuum geometry. Positivity of the relative entropy implies then that the inequality ∆ H C ≥ ∆S , (C.6) must be satisfied if the non-vacuum geometry under question allows for a consistent quantum-mechanical interpretation as the holographic dual of the state ρ.
A direct holographic computation where the vev's of the two energy-momentum in (C.5) are evaluated explicitly considering the subleading mode of the dual metric, shows that for the pumping solution and for any opening angle θ 0 of the cap, ∆ H C ≤ 0. On the other hand, it is possible to show that ∆S ≥ 0, both by a perturbative computation at α b 1 as well as numerically for finite α b . Hence, the negative energy density associated to the pumping solution rises an apparent violation of the above formula. Note however that the holographic computation needs probably to be reconsidered and refined. Indeed, we have to deal properly with the introduction of the background source φ 0 = α b t. Let us linger on this important point more extensively. The deformation of our original CFT by means of the new time-dependent coupling implements an exactly marginal flow in theory space. As a consequence, the straightforward application of the GPKW prescription 18 W ren (γ µν , φ 0 ) = S ren (γ µν , φ 0 ) , (C.7) to the pumping solution would allow us only to compute the vev of the stress-energy operator defined with the linearly rising scalar source. While the stress-energy operators appearing in (C.5) are both defined with the scalar source set to a constant value. In other words, consider the holographic quench that produces the pumping solution at t → ∞. This corresponds to the time-dependent deformation introduced by the background field φ 0 (t), such that φ 0 (t ≤ 0) = 0, lim t→∞ φ 0 (t)/t = α b . At a generic t > 0, the relation (C.7) would be computing the expectation value of the energy-momentum tensor of the deformed theory, and not of our original theory. These two operators, which we choose to denote respectively asT , are generically different, because of the nontrival deformation of our initial CFT due to the marginal coupling. Relation (C.7) guarantees then access to T [φ 0 ] µν t , but not to T [φ 0 =0] µν t . Therefore the procedure we outlined to compute S(ρ||σ) holographically cannot in general be applied directly to our case. We would need additional information to know precisely how the two operators JHEP05(2017)141 µν are related by the time-dependent deformation; for instance, access to the microscopic description of the dual CFT would clarify the point.
It is interesting to note that we can invert the logical flow and use the potential paradox implied by violating (C.6) to guess some features of the deformed theory. Suppose the deformed and undeformed energy-momentum operators satisfy a relation of the form 19 In the pumping solution, at sufficiently late values of time, O φ t = 0 and hence we would have In such a case, the above-mentioned holographic computation would give the correct result and the l.h.s. of equation (C.6) would be negative, violating the entropy inequality. At this point, we refrain from reaching provocative conclusions, given the uncertainties that we have spelled out concerning the correct way of computing the left hand side of (C.6).
We would like to mention at this point the reference [21] that appeared the same day as ours in which they consider a similar marginal scalar sourced linearly in time. They also find a discrepancy in the so called Firt Law of Entanglement Entropy, which is (C.6) in the limit of infinitesimal deformation. Altogether this points out an interesting direction of future research.
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