On some universal features of the holographic quantum complexity of bulk singularities

Journal of High Energy Physics, Jun 2018

Abstract We perform a comparative study of the time dependence of the holographic quantum complexity of some space like singular bulk gravitational backgrounds. This is done by considering the two available notions of complexity, one that relates it to the maximal spatial volume and the other that relates it to the classical action of the Wheeler-de Witt patch. We calculate and compare the leading and the next to leading terms and find some universal features. The complexity decreases towards the singularity for both definitions, for all types of singularities studied. In addition the leading terms have the same quantitative behavior for both definitions in restricted number of cases and the behaviour itself is different for different singular backgrounds. The quantitative details of the next to leading terms, such as their specific form of time dependence, are found not to be universal. They vary between the different cases and between the different bulk definitions of complexity. We also address some technical points inherent to the calculation.

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On some universal features of the holographic quantum complexity of bulk singularities

HJE On some universal features of the holographic quantum complexity of bulk singularities Stefano Bolognesi 0 1 3 5 Eliezer Rabinovici 0 1 3 4 Shubho R. Roy 0 1 2 3 0 Hyderabad , Kandi, Sangareddy 502285, Medak, Telengana , India 1 91904 , Israel 2 e Witt patch 3 Largo Pontecorvo , 3, Ed. C, 56127 Pisa , Italy 4 Racah Institute of Physics, The Hebrew University of Jerusalem 5 Department of Physics “E. Fermi”, University of Pisa and INFN Sezione di Pisa We perform a comparative study of the time dependence of the holographic quantum complexity of some space like singular bulk gravitational backgrounds. This is done by considering the two available notions of complexity, one that relates it to the maximal spatial volume and the other that relates it to the classical action of the WheelerWe calculate and compare the leading and the next to leading terms and find some universal features. The complexity decreases towards the singularity for both definitions, for all types of singularities studied. In addition the leading terms have the same quantitative behavior for both definitions in restricted number of cases and the behaviour itself is different for different singular backgrounds. The quantitative details of the next to leading terms, such as their specific form of time dependence, are found not to be universal. They vary between the different cases and between the different bulk definitions of complexity. We also address some technical points inherent to the calculation. Gauge-gravity correspondence; Spacetime Singularities 1 Introduction 2 3 4 1 Time dependence in the boundary metric: Kasner and Topological Time dependence in the bulk: De Sitter crunch Conclusion Introduction of the order of exp(S). We remark that the claim for the existence of a maximum value – 1 – of the complexity resides in the attempt to reconcile the continuous structure of the space of all quantum states with the manner by which each such state is reached by a discrete and finite number of prescribed operations. This is done by assigning an arbitrary required accuracy for declaring a particular approximation of the target state as successful. Without such a cutoff the complexity defined in this way has no upper bound. Some authors, [5] and references therein, have been flirting on and off with considering metrics and geodesics on the space of states with which the system would have a universal maximum complexity, however at this stage neither this nor a dynamical cutoff were identified. The need for an arbitrary cutoff has not been removed and the states of a Quantum Field Theory have indeed a maximum complexity for given values of the entropy and the cutoff. For other recent developments on the definition of complexity in QFT see [9–12]. There are presently two suggestions, each with its own motivation, as to what the complexity of a quantum boundary state should be given by in the bulk. One is that is should be, up to some proportionality coefficient, the volume of the maximal spatial surface extending into the bulk and terminating on the boundary at the spacial slice on which the boundary quantum state is defined [6]. This is referred as the complexity proportional to volume (C ∝ V) conjecture. The other is [7, 8] is that the complexity is proportional to the classical value of the action in a WdW patch. The so called (C ∝ A) conjecture. One takes the spatial slice on the boundary on which the state is defined. Then one considers the union of all possible spatial slices which extend into the bulk and terminates on the same spatial slice at the boundary. The union forms a sub-set of the bulk called the Wheeler-de Witt (WdW) patch. The Einstein-Hilbert (EH) action evaluated on this patch, with the inclusion of the proper York-Gibbons-Hawking (YGH) boundary term, is conjectured to be proportional to the complexity. The spatial slice of maximal volume considered for the C ∝ V conjecture is contained in the WdW patch but now it does not play any preferential role with respect to the others. Be the complexity of a state what it may be on the boundary CFT and be the corresponding bulk quantity what it may be for the purpose of the study of singularities it is one of its features, its time dependence, that is proposed as a diagnostic tool on its own. It is on the universal features of this quantity that we focus on in this paper. Based on examples [7, 8] it is argued that as long as the complexity of a state increases in a black hole context no singularity is encountered. In addition it is claimed that this result is robust and remains valid when small perturbations are added to fine tuned states such as the thermofield double [13]. On the other hand if the complexity does decrease in time the state may well encounter a singularity that one could associate with the formation of a firewall like obstacle. However this evolution is claimed, on the basis of examples, not to be robust, once small perturbations are added to such a system the potential formation of a firewall type singularity is delayed for at least a time of the order exp(S). There are other circumstances in which the complexity is expected to decrease [ 14 ]. The Poincare recurrences which occur in QFTs, when they obey certain conditions, after the passage very large times of order exp(exp(S)), bring down the complexity with them. This decrease need not signal necessarily an approach to a singular configuration. This decay is indeed not robust itself but once one decides on what the Hamiltonian and the state are these decays will occur again and again with Poincare time intervals. – 2 – In addition to the black hole case it was found, using the C ∝ V conjecture, that the complexity does decrease as the system approaches some pre-engineered classes of time dependent singularities [ 17 ]. These are intriguing singularities of the type one may be able to coexist with. This result could be expected and is robust for BKL [ 15, 16 ] type singularities but the generality of this feature is less clear and was obtained using the extremal volume prescription to calculate the complexity. Given the scarcity of the present knowledge on the nature of these singularities we explore here if this feature depends on the well motivated, but particular, bulk quantity which was conjectured to be associated with the QFT complexity. In this work we obtain the complexity by using the C ∝ A prescription. This way of evaluating the complexity presents its own challenges. The work will be largely of a technical nature. The result that we find is qualitatively similar the one obtained with the C ∝ V, in particular complexity always decreases toward the crunch. The quantitative details and in particular the specific form of time-dependence of the complexity are instead different. Complexity is a UV divergent quantity so its regularization is necessary, as we discussed it is after the time dependence of the complexity that we are after. Both the C ∝ V and C ∝ A conjectures are sensitive to this divergence and a way to deal with it is to introduce a UV cutoff close to the boundary. For the C ∝ A there is computational difficulty. The boundary of the WdW patch is a light-like sub-manifold with joints. Both issues, being light-like and having joints, means that the YGH boundary term must be properly defined. This problem has been recently discussed in [ 18–20 ]. For the present paper we take a different approach to this problem (see also [ 8, 21 ]). Since we have anyhow to UV regularize the WdW patch, we use this opportunity to introduce a particular regularization that makes the WdW boundary time-like and also smooths-out the joints. In this way we can compute the YGH term with no ambiguities. There are two distinct types of time-dependent backgrounds. For the first type time dependence is explicit in the UV part of the metric. This case corresponds to some time dependent marginal operator in the dual field theory. The Kasner metric and the topological crunch are two examples of this type and we will study them in detail. In those cases also in the UV divergent part of the complexity is time-dependent. For the second class the UV metric has no explicit time dependence but the whole bulk metric does. The de Sitter crunch model is the specific example of this type that we will consider here. In those last cases the divergent piece of the complexity is free from any time dependence and the time derivative of the complexity is a finite quantity. The paper is organized as follows. In section 2 we consider the cases of time dependence on the boundary. In section 3 we consider the bulk time dependence. We conclude in section 4. 2 Time dependence in the boundary metric: Kasner and Topological crunch In this section we perform a comparative calculation and study of the complexity and its time dependence as obtained according to two of its different bulk definitions. This for – 3 – two cases engineered in such a way that the world volume of the boundary theory itself is singular. For each definition and each class of metrics we obtain the leading and next to leading terms. The result will coincide with those of [ 17 ] for the leading term when the volume prescription is adopted, this for both types of metrics. We do this by studying two cases in which the metric on the world-volume of the dual field theory has the form with i, j = 1, . . . , d. The UV boundary is set at z = 0 and the world-volume frame where the CFT is realized is ds2CFT = −dt2 + hij (t, x)dxidxj . All cases we consider satisfy everywhere z2 −dt2 + dz2 + hij (t, x)dxidxj R − 2Λ = − 2(d + 1) L2 The first definition of complexity is C ∝ V where V is the spatial slice with maximal volume whose boundary is at a fixed time t = t∗. We consider any possible spatial slice defined by ΛUV = 1 zUV . t = f (z, xi) – 4 – d(2dL+21) is the cosmological constant. This is true whenever the world-volume The first specific example is that of the Kasner metric. The Kasner metric is of the hij (t, x) = diag t 2p1 l , . . . , t 2pd ! l X pi = X pi2 = 1 . i i and l is a dimensional scale. The second specific example is that of the so called topological crunch. The topological crunch, close to the boundary, is of the form (2.1) with where Λ = − frame is Ricci flat. form (2.1) with with the relation (2.1) (2.2) (2.3) (2.4) (2.5) (2.6) (2.7) hij (t, x)dxidxj = l2 dΩ2d−1 + cos2 dφ2 when the CFT world-volume goes to zero, and this is t = 0 for Kasner and t = ±l π2 for the topological crunch case. The latter is called topological because locally the metric (2.1) with (2.5) is always the same as AdSd+2. We will perform the computations using the generic form (2.1) and then adapt to the specific cases at the end. Complexity, in any of its forms, has always a divergent term that is due to the contribution coming from close to the UV boundary. This can be regularized by introducing a UV cutoff ΛUV related to a minimal value of the z coordinate with the property z→0 lim f (z, xi) = t∗, ∀xi . Since the spaces we are considering are homogeneous in xi, we can always restrict to the case ∂if = 0 everywhere, so from now on we take f (z) to be just a function of z. The induced metric on this space slice is L2 ds2 = z2 (1 − (∂zf )2)dz2 + hij(f, x)dxidxj and the space volume is then where we indicate V = Z dzdVx zd+1 Ld+1 p(1 − (∂zf )2) h(f (z), x) dVx = dx1 . . . dxd and h(t, x) = det hij(t, x) . The expansion of the metric determinant is h(t, x) ≃ h(t∗, x) + (t − t∗)h(t∗, x)hij(t∗, x)∂thij(t∗, x) + . . . Note that for spaces homogeneous in x the quantity hij(t, x)∂thij(t, x) does not depend on x so we will denote it simply as hij∂thij(t). The Euler-Lagrange equation for f (z), after some simplification, becomes ∂z2f = 1 − (∂zf )2 (1 + d)∂zf z − 2 1 hij∂thij(f (z)) By expanding near z = 0 and solving the equation in a power series of z we find that f (z) goes to t∗ with zero derivative The space volume is dominated by the following UV divergent term: f (z) = t∗ + α(t∗)z2 + . . . . V ≃ ≃ Z 1/ΛUV ΛdUVLd+1 Z d dz Z Ld+1 dVx zd+1 Note that the leading divergence is proportional to ΛdUV and does not depend on α(t∗) or any of the sub-leading terms in the expansion of (2.14). Note also that this term is proportional to the boundary space volume R dVx ph(t∗, x) and this is what provides the dependence with respect to anchored time t∗. We next turn to the sub-leading divergencies which are affected by the coefficient α(t∗) in (2.14). Continuing the power expansion of the equation (2.13) it can be found, for d > 1 α(t∗) = hij∂thij(t∗) 4d . – 5 – (2.8) (2.9) (2.10) (2.11) (2.12) (2.13) (2.14) (2.15) (2.16) HJEP06(218) d Z dVx ph(t∗, x) = 2πldVSd cos t l and hij ∂thij = − 2l tan tl . The volume is then d V = ΛUV Ld+12πldVSd cos tl + ΛdU−V2 Ld+1π(d − 1)ldVSd sin2 t l d2(d − 2)l2 cos tl + . . . (2.21) (2.18) (2.19) (2.20) Z dVx ph(t∗, x) = V t l where V is an IR cutoff for the spatial volume in xi. Moreover for the Kasner metric we have hij ∂thij = 2t . The volume is then d V = ΛUV Ld+1V t dl + ΛdU−V2 L2dd+21((dd−−21))lVt + . . . For the leading divergence we recover the result of [ 17 ]. Note that the leading order divergent term is linear in t and it is decreasing in time till it would have vanished at the singularity t → 0. The validity of the approximation breaks down as one reaches to Planckian and string scale distances tUV ≃ ΛU1V . This is also the time by which the sub-leading divergent term becomes of the same order of the leading one. The complexity decreases at a rate linear in time as long as the approximation is valid. A linear dependence of the complexity on time was obtained in the eternal black hole case among other ones [6, 7], although in the latter case it was for a non-divergent piece of the complexity. In the Kasner case the linear dependence follows directly from the relation (2.4) and is not a universal feature as we are going to see next. For the specific case of the topological crunch we have Note that α(t∗) is uniquely determined once the first constant of integration t∗ is decided. The second constant of integration appears at orders higher than z2 in the power expansion for f (z). The sub-leading divergent term of the volume depends only on α(t∗) and is V = O(ΛdUV) + ΛdU−V2 Ld+1(d − 1)(hij ∂thij (t∗))2 Z 8d2(d − 2) dVx ph(t∗, x) + . . . (2.17) Sub-leading divergent terms are present whenever hij ∂thij 6= 0. where O(ΛdUV) is the leading term (2.15) while the sub-leading term is of order O(ΛdU−V2). For the case of the Kasner metric we have For the leading divergence we again recover the result of [ 17 ]. As in the Kasner metric case the complexity vanishes towards and close to the crunch, but the time dependence is no longer linear in this case. The considerations to be applied in constraining the proximity of the time to the singularity while retaining the validity of the approximation are similar to those presented for the Kasner metrics. We will now spend a moment on an issue of the C ∝ V not discussed previously. When we have only one boundary for the CFT frame, a quantum state is defined once – 6 – we specify one number, the time t∗ when we take the spatial slice. The maximal volume equation (2.13) on the other hand is a second order differential equation and needs two conditions to select a particular volume that extends in the bulk. This second boundary condition, for d > 1, appears in the expansion (2.14) to higher order than O(z2), so it does not affect either the leading (2.15) or the sub-leading (2.17) divergences of the volume. Nevertheless, if we want to make sense of the C ∝ V conjecture we need to specify this condition and select one particular volume. If we take hij constant, the generic solution of (2.13) with f (0) = t∗ is 1 d + 2 f (z) = t∗ + zψ βzd+1 = t∗ + βzd+2 + . . . (2.22) where ψ is some known function expressed in terms of an hypergeometric function and β is the second integration constant which appears only at order zd+2 in the expansion. All of those solutions are locally maximal volume surfaces and the union of all of them gives the WdW patch. If we want to select a particular one, in order to associate it to the complexity of the boundary state, a natural choice would be the constant solution, β = 0, equal to t∗ everywhere. When hij depends of time this choice becomes less obvious. Let’s take for example the case of Kasner and we plot in figure 1 various solutions of the maximal volume equation (2.13) with f (0) = t∗. As before the union of all the solutions gives the WdW patch. All solutions, save one, become asymptotically null at large z like f (z) = z + const or f (z) = −z + const. The special one that divides the two types of solutions is a natural candidate to be associated at the boundary state. Its slope at z → ∞ in neither 1 nor −1 and in general depends on the anchored time t∗. For the purpose of the present paper this is not an urgent issue since all those solutions share the same quadratic expansion and thus have the same leading and sub-leading divergences. So we will not discuss this issue any further here. We now turn to obtain the complexity as given by the definition C ∝ A where A is the action of the WdW patch anchored at t = t∗ on the UV boundary. We need to regularize the action and to this end we smoothen-out the boundary of the patch. Our choice is to – 7 – WdW patch 1 t∗ ΛUV take, as in figure 2, the region of space-time delimited by the following hyperbole . As ΛUV → ∞ we recover the full WdW patch. This regularization achieves two goals simultaneously. First it regularize the UV divergence. Second the boundary of the regularized patch is now a smooth time-like boundary with no joints: this allows the computation of the boundary gravitation action without any ambiguities. The total action is given by the Einstein-Hilbert (EH) term with the cosmological constant plus the boundary York-Gibbons-Hawking (YGH) term A = AEH + AYGH = 1 16πG Z WdW √−g (R − 2Λ) + ǫ Z where ǫ = ±1 according if the boundary is time-like or space-like. The boundary of the WdW is a null hypersurface, but we will consider it as a limit of a time-like submanifold (2.23). So from now on we will assume ǫ = +1 and |γ| = −γ. The EH term evaluated on the regularized patch is AEH = = 16πG 1 1 16πG Z Z Z ∞ dt Z dVx dt √1+Λ2UV(t−t∗)2 dz We are interested in capturing the dominant divergent piece of the action. So we take g to be equal to its boundary value at t = t∗: AEH ≃ − 8πG Γ d+1 2 Note that this term is proportional to the boundary space volume and the divergence is proportional to ΛdUV. The sign of AEH is negative because of the sign of R − 2Λ , but it will be overcome by the boundary term which turns out to be positive. To see to the final answer the reader can go directly to (2.35) and (2.36). In the following we present the technical details needed for obtaining AYGH. We need to compute some useful geometrical quantities before the evaluation of the boundary YGH action. The components of the connection we will use later are: Γzzz = − z , 1 Γtzt = Γttz = Γtzt = − z , 1 Γizj = 1 z hij , Γitj = 1 2 ∂thij . (2.27) The boundary (2.23) is a time-like sub-manifold and we can choose to parameterize it with the coordinates xa : t, xi. It is defined by the following embedding: 1 q The Jacobian of the embedding eaμ = ∂∂xxμa is ett = 1 etj = 0 etz = q ejz = 0 ΛUV(t − t∗) 1 + Λ2UV(t − t∗)2 eit = 0 eij = δji . K = γabeaμebν∇μnν = 1 L d − 2 1 hij∂thij(t − t∗) q 1 + (t − t∗)2Λ2UV . – 9 – The induced metric γab on the boundary manifold xa is The outward unit normal is ds2 = L2 z2 1 − (t − t∗)2Λ2UV + 1 dt2 + hij(t, x)dxidxj . nt = q LΛ2UV(t − t∗) 1 + Λ2UV(t − t∗)2 nz = −LΛUV with eaμnμ = 0 and nμnμ = 1. The final result will not depend on the specific way nμ is extended outside the boundary. The covariant derivative is ∇μnν = ∂μnν − Γρμνnρ, and the components are ∇tnt = ∂tnt + ∇znz = nz z nz z n t z ∇znt = ∇tnz = 1 1 ∇inj = − 2 ∂thijnt − z hijnz . We can now compute the extrinsic scalar curvature of the boundary sub-manifold (2.29) (2.30) (2.31) (2.32) (2.33) The YGH boundary term is then AYGH = As before, to extract the dominant divergent term we take g to be equal to its boundary value at t = t∗: AYGH ≃ 8πG ≃ 8πG The final result for the dominant divergent term of the action is then the sum of (2.26) and (2.35): The coefficient is always positive for d > 1 despite the EH being negative, the positive YGH term is always the dominant contribution. The result for the leading UV divergence of the complexity is thus the same obtained for the C ∝ V in (2.15). In both cases the complexity decreases towards the singularity in the region of validity of the approximation. We next study the sub-leading divergences. For this we need the expansion of the metric determinant up to the second order around t∗ where H1(t) and H2(t) are given by h(t, x) ≃ h(t∗, x) 1 + (t − t∗)H1(t) + (t − t∗)2H2(t) + . . . 1 2 H1(t) = hij ∂thij , H2(t) = hij ∂t2hij − hjl∂thlkhki∂thij + H12 . (2.35) (2.36) (2.37) (2.38) (2.39) (2.40) (2.41) The expansion for the EH terms (2.25) gives AEH ≃ O d ΛUV AYGH ≃ O d ΛUV + LdΛd−2 √πΓ d2 − 1 UV − 128πG where O(ΛdUV) is the leading term (2.35). The final result is A ≃ O d ΛUV + LdΛd−2 √πΓ d2 − 1 UV 128πG where O(ΛdUV) is the leading term (2.36). 2H2 − H12 Z dVx 2(d − 1)H2 − (d + 1)H12 Z dVx det hij (t∗, x) where O(ΛdUV) is the leading term (2.26). The expansion for the YGH terms (2.34) gives q q For the Kasner metric H1 = 2t , H2 = t22 and the action is then . In this case, due to the fact that √ h is linear in t, we essentially recover the same result see some difference in the subleading divergence because √ we had for the volume prescription (2.19). For the case of topological crunch instead we h is not linear in time. In the latter case we have H1 = − 2l tan tl , H2 = l22 tan2 t l − 1 and the action is HJEP06(218) We see that the subleading divergence is different from the one obtained with the volume prescription (2.21). In the next part of the paper we will test if the result we have found in this section, that the main features of the complexity for space like singularities, are independent on the choice among the two bulk prescriptions, is valid also for the de Sitter case. 3 Time dependence in the bulk: De Sitter crunch We next turn to cases in which a Big Crunch occurs semi-classically in the bulk. This can be represented by either a boundary theory, with particular time dependent relevant deformations, living on a time independent world volume which exists for only a finite time (denoted EF) or by a conformally related time independent boundary system living on an expanding de Sitter world volume (denoted by dSF). This duality was studied in [ 1, 3 ]. In this case the time derivative of the complexity is a finite quantity, both for the volume and the action prescriptions. It does not depend on the UV regularization. We first make a more generic analysis in the absence of divergent terms in the time derivative of the complexity. Consider a metric is of the form (3.1) (3.2) L2 z2 ds2 = dz2 + hμν (t, x)dxμdxν with µ, ν = 0, 1, . . . , d and the UV boundary is at z = 0. The expansion of the metric near the boundary is in general of the following form hμν = h(μ0ν) + z2h(μ2ν) + · · · + zdh(μdν) + zd log z2h(μdν) + . . . For the EF case one has h(μ0ν) equal to the EF metric and the entire time dependence is due to a domain wall moving in the bulk. We thus consider the case in which h(μ0ν) is static while sub-leading terms in the expansion (3.2) may contain information about the time dependence. Let’s assume for generality that h(μ2νk)(t, x) is the first term to contain a time dependence, then the contribution to the complexity from the term (2.41) is A ≃ O d ΛUV + O ΛdU−V4k So, for small enough dimension d < 5 we do not have any divergent terms.1 In this case to compute the time dependence of the complexity, which is a finite term, we have to consider the full metric and also the precise shape of the WdW patch; considering only the asymptotic form of the metric close to the UV is not enough. This leads us to perform the computations on a case-by-case basis. We now consider in detail the de Sitter crunch in the case that the thin wall approximation is valid. This occurs when the boundary field theory in its dSF coordinates contains a negative relevant operator whose coefficient is much larger than its expansion rate [ 1, 3 ]. The metric in the UV is AdS+ with curvature length l+ = 1 which we fix to one for convenience (3.3) (3.4) (3.5) (3.6) (3.7) (3.8) ds2 = dρ2 + sinh2 (ρ) −dτ 2 + cosh2 (τ )dΩ2d This is valid for ρ > ρW where ρW is the position of the domain wall. The metric on the other side of the wall ρ < ρW is AdS− with a smaller curvature length l− < 1. In order to match the two metrics at the same value of ρ we need to perform some rescaling of the standard form. The expression for the interior metric is with ds2 = l−2α2dρ2 + l−2 sinh2 (αρ) −dτ 2 + cosh2 (τ )dΩ2d 1 ρW α = arcsinh sinh (ρW ) l− > 1 This is valid for ρ < ρW . In this coordinate choice the two metrics are patched so that they are continuous at ρ = ρW . The position of the wall ρW is constant in the time τ . In the dual field theory this correspond to an RG flow between two different CFT’s. The limit we are discussing is that of the thin-wall approximation. Now we focus on the exterior region, the one that extends to the UV. By changing coordinates to the metric (3.4) becomes r = sinh (ρ) cosh (τ ) cos (t) = cosh (ρ) q dr2 ds2 = (1 + r2) − 1 + r2 dt2 + r2dΩ2d 1Rember that d is the number of space dimensions on the boundary, for example d = 3 for AdS5. For d ≥ 5, so from AdS7 onward, a bulk time dependence of the metric can in general provide a time-dependent divergent piece in the action trough its tail at z → 0. We will not consider those cases in the present paper. and the wall is not static but follows the trajectory r(t)W = cosh2 (ρW ) cos2 (t) At the time t → π2 where r(t)W → ∞ we have a bulk crunch. We will work in this EF frame where the metric does not depend on time, although it exists only for a finite time, and the bulk crunch is visible on the boundary. Note that the metric time dependence is only through the wall trajectory. In the UV the metric is constant. We then have consider the interior part AdS− with L = l−. We first rewrite (3.5) the The domain wall is then at ρW = αρW . Then we change coordinates to r = sinh (ρe) cosh (τ ) e cos et = q cosh (ρe) The wall trajectory is these coordinates is dr2 e ds2 = l−2 1 + r2 − 1 + r2 det2 + r2dΩ2d e e e re(et)W = cosh2 (αρW ) cos2 et 1 ! 2 − 1 The metric is AdS− in the region re ≤ re(et)W . The crunch is at et → π2 where re(et)W → ∞. In what follows we will use two different coordinate systems: for the exterior (3.8) and for the interior (3.13). The two patches are connected at the wall trajectory which is different in the two coordinates systems, respectively (3.9) and (3.14). This is the price we pay in order to have the two metrics writen in a simple form. When passing from one patch to the other we have to change also coordinates. A point on the domain wall in AdS+ at time t and radius r(t)W in the AdS− patch will be seen at time and radius  et = arccos  q cos (t) cosh (αρW ) cos2 (t) + ssininhh((αρρWW)) cosh2 (ρW ) − cos2 (t)   , r = e r l− . (3.15) We work in the thin wall approximation. In general we can construct a wall with a scalar field and a suitable potential with two minima, the values at the two minima correspond to the cosmological constant at the two sides of the wall. We can then scale the microscopic parameters and send the wall thickness to zero while keeping the tension fixed. Assuming that the curvature in the middle of the wall remains of the same order (3.9) (3.10) (3.11) (3.12) (3.13) (3.14) V+ = The total volume is then V = V+ + V− = VSd ld+1 Z reW (t∗) − dr √ r d 1 + r2 + The derivative with respect to t∗ is free from UV divergence and, using (3.15), it becomes ddtV∗ = VSd dt drW rW (t∗)d  q 1 1 + rW (t∗)2/l−2 − p1 + rW (t∗)2  1 This is always negative for l− < 1 and t > 0 which means that complexity(volume) is decreasing going toward the crunch. For t∗ → π2 we have ddtV∗ = VSd coshd (ρw)(−1 + l−) We now calculate the Complexity using the WdW prescription. For this task it is convenient to change again coordinates !  of the cosmological constants, the thin wall limit allows us to neglect the terms from the action coming from the wall itself. The space volume anchored at t = t∗ in the UV part is The space volume anchored at t∗(t∗) (the relation is given by (3.15)) in the IR part is r = cot(z) π with 0 ≤ z ≤ 2 . The metric (3.8) becomes ds2 = 1 + cot2(z) −dt2 + dz2 + The domain wall trajectory is Close to the crunch In these coordinates the WdW patch is delimited by zW (t) = π 2 − arctan r(t)W zW (t) ≃ cosh (ρW ) z = |t − t∗| (3.16) (3.17) (3.18) (3.19) (3.20) (3.21) (3.22) (3.23) (3.24) (3.25) t∗ zW (t) z A AdS+ HJEP06(218) (3.26) (3.27) (3.28) (3.29) (3.30) (3.31) show the WdW patch anchored at t∗ enclosed in this region and the intersections zA(t∗) and zB(t∗). Intersection with the domain wall trajectory is at (tA(t∗), zA(t∗)) and (tB(t∗), zB(t∗)) with tB(t∗) > tA(t∗) and intersections are zA(t∗) > zB(t∗) for t∗ > 0 In general we cannot solve analytically for zA(t∗) and zB(t∗). Close to the crunch the two tA(t∗) ≃ tB(t∗) ≃ π cosh (ρW )t∗ − 2 cosh (ρW ) − 1 cosh (ρW )t∗ + π2 cosh (ρW ) + 1 zA(t∗) ≃ cosh (ρW ) − 1 zB(t∗) ≃ cosh (ρW ) + 1 The geometry of AdS+ with the WdW patch is pictured in figure 3. Now we compute the action of the WdW patch anchored at the UV boundary t∗. The EH term is AEH+ = = − 1 16πG Z WdW (d + 1)VSd Z tB 8πG tA √ dt Z zW (t) |t−t∗| dz cotd(z) 1 + cot2(z) where we used R − 2Λ = −2(d + 1). The derivative with respect to t∗ is The boundary YGH term is obtained next . The metric (3.41) is with dAEH+ = dt∗ VSd 8πG cotd+1(zB) − cotd+1(zA) ds2 = g(z) −dt2 + dz2 + f (z)hij (x)dxidxj g(z) = 1 + cot2(z) f (z) = cot2(z) and hij the metric of Sd. The component of the connection of the metric that we need are: Γzzz = g′(z) 2g(z) Γtzt = Γttz = Γtzt = g′(z) 2g(z) f ′(z) Γizj = − 2g(z) hij . We use the same time-like hyperboloid as before and then send the cutoff to infinity to obtain the light-like boundary of WdW. The boundary is defined by (2.28). The induced metric γab on xa is ds2 = − (t − t∗)2Λ2UV + 1 g(z) dt2 + f (z)hij(t, x)dxidxj The Jacobian of the embedding eaμ = ∂∂xxμa is the same as in (2.29). The outward unit normal is nt = pg(z)ΛUV(t − t∗) q nz = − g(z) 1 + Λ2UV(t − t∗)2 . The components of the covariant derivative different from zero are and the extrinsic curvature is then ∇znt = ∂znt − 2g(z) nt ∇znz = ∂znz − 2g(z) nz g′(z) g′(z) K = γabeaμebν∇μnν = − g(z) 2 ΛUV dzΛUVf ′(z) 1 − 2f (z)g(z) 12 − ΛUVzg′(z) 2g(z) 2 3 . Putting all these together allows to be obtain the YGH boundary term: AYGH+ = 1 Z √−γK = VSd Z 8πG dt d g(z) 12 f (z) 2 (t − t∗)2Λ2UV + 1 2 1 K The terms is simplified by removing the cutoff, that is sending ΛUV → ∞ AYGH+ = − 16πG tA VSd Z tB dtf (z) 2 d−2 2f (z) + df ′(z) + f (z)g′(z) g(z) where z = |t − t∗|. The time derivative takes contributions only from the boundary of the boundary since the bulk of AdS+ in time independent and is dAYGH+ = − 16πG VSd dt∗ ddztB∗ f (zB) 2 d−2 2f (zB) + df ′(zB) + f (zB)g′(zB) g(zB) + ddztA∗ f (zA) 2 d−2 2f (zA) + df ′(zA) + zA f (zA)g′(zA) g(zA) . (3.39) zB dinates as and the metric (3.13) is then The domain wall trajectory is AEH− = = − 1 16πG Z WdW (d + 1)VSd l−d 8πG e cotd(z) 1 + cot2(z) √ −g(R − 2Λ) Z etA etmin e Next we evaluate the WdW action in AdS− interior. It is convenient to change coorr = cot (ze) e ds2 = l−2 1 + cot2(z) e −det2 + dz2 + e e e dΩ2d zfW (te) A AdS− π π HJEP06(218) (3.40) (3.41) (3.42) (3.43) (3.44) ! dz e (3.45) together with zW (et). The minimun and maximum values of et are e z = −et+ etA + zA e e z = et− etB + zB e e etmin = etA + zeA − 2 etmax = etB − zeB + π 2 The geometry of AdS− is pictured in figure 4. The action of the WdW patch that anchored at UV boundary t∗. The EH term is zW (et) = e 2 − arctan re(et)W Intersection with the domain wall trajectory is at etA, zeA and etB, zB to be obtained e using (3.15) and (3.40) from the corresponding values in AdS+ which are (tA(t∗), zA(t∗)) and (tB(t∗), zB(t∗)). In these coordinates the WdW patch is again delimited by Z π/2 dt e −et+etA+zeA dz + e Z etB e tA Z π/2 dt e zeW (et) e dz + Z etmax e tB Z π/2 dt e et−etB+zeB where we used R − 2Λ = − l− dAEH− = − 8πG dt∗ VSd l−d d etB − zeB cotd+1(zeB) − dt∗ d etA + zA cotd+1(zeA) e dt∗ ! (3.46) The YGH boundary term is The time derivative is dAYGH− = dt∗ AYGH− = − 16πG VSd l−d f (z) 2 e d−2 Z etA etmin 2f (z) + z e Z etmax ! e tB dt e e + df ′ (ze) + f (ze) g′ (z) e h′ (z) e VSd l−d 16πG dzA + e f (zeA) 2 dt∗ d−2 dzB dt∗ e f (zeB) 2 d−2 2f (zeA) zA e 2f (zeB) zB e + df ′ (zeA) + + df ′ (zeB) + f (zeA) g′ (zeA) h′ (zeA) f (zeB) g′ (zeB) h′ (zeB) Finally we can now sum all contributions to the derivative of the action which is the sum of the four terms (3.29), (3.39), (3.46), and (3.48). We present a numerical evaluation of ddtA∗ in figure 5. The plots are done for the specific values of d = 2, l− = .9 and ρW = .5. We also plot the asymptotic formula close to the crunch (3.50). The time derivative is negative and becomes larger close to the singularity. That is qualitatively the same behaviour as obtained for the volume prescription (3.20) ddAt∗ = dAEH + dt∗ dAYGH dt∗ dA dt∗ ∝ 1 The degree of approach to the singularity is not same as is shown in figure 6 where we plot the ratio ddtV∗ / ddtA∗ . However the origin of the negative sign is the same in both cases, it follows because l−, the curvature length in the IR, is smaller than l+ = 1 which is the curvature length at the UV. This allows one to identify that the source of the decrease in complexity is the result of the renormalization group flow, there are less degrees of freedom in the IR than in the UV. Thus both definitions suggested for the Holographic complexity capture the same physical aspects as far the decrease of complexity in these classes of singular cases. 4 Conclusion Different motivations lie behind each of the two suggestions for the bulk quantity which corresponds to the quantum holographic complexity of the boundary state. Given that one does not have yet a precise and universal definition of complexity in quantum field theory itself, both can be considered as suggestive holographic probes for the notion of how complex is a quantum state. There is no a priori reason for them to coincide in a (3.47) HJEP06(218) (3.48) (3.49) (3.50) generic situation and indeed, while we have shown that the degree of divergence is the same, we have shown also that there are quantitative differences. In some cases only for the next to leading term and in other cases for both the leading and next to leading term. The quantitative behaviour itself, even when the same for both suggestions, differed according the type of singular background. However both deliver the same verdict as far as the manner in which the complexity of several classes of time-dependent holographic backgrounds, which have crunch singularities, evolves. The complexity decreases. Another universal feature that we have found that the time derivative of the complexity contains a UV divergent part if the boundary metric depends explicitly on time while it is finite otherwise. Another pattern emerged from the action calculation. For the cases in which the time dependence character was driven mainly from a divergent term , it was the boundary YGH term which determined the sign of the time derivative while for the case where the time dependence was driven by a finite term in the evaluation of the complexity it was the EH volume term which dictated the final sign. The universality we have found adds credence to the identification of the physical source of Complexity decrease given in [ 17 ]. This leaves us with yet one more indication that for some probes space like singularities may less of a bite than expected. Acknowledgments We thank J. Barbon and J. Martin for useful discussions. We thanks Jie Ren for collaboration in the early stage of this project. S. B. work is supported by the INFN special research project grant GAST (“Gauge and String Theories”). The work of E. R. was partially supported by the American-Israeli Bi-National Science Foundation. The work of E. R. and S. R. was partially supported by the Israel Science Foundation Center of Excellence and the I Core Program of the Planning and Budgeting Committee and The Israel Science Foundation The Quantum Universe. The work of S. R. is supported by the IIT Hyderabad seed grant SG/IITH/F171/2016-17/SG-47. Open Access. This article is distributed under the terms of the Creative Commons Attribution License (CC-BY 4.0), which permits any use, distribution and reproduction in any medium, provided the original author(s) and source are credited. [3] J.L.F. Barbon and E. Rabinovici, AdS Crunches, CFT Falls And Cosmological Complementarity, JHEP 04 (2011) 044 [arXiv:1102.3015] [INSPIRE]. [4] J.L.F. Barbo´n and E. Rabinovici, Conformal Complementarity Maps, JHEP 12 (2013) 023 [arXiv:1308.1921] [INSPIRE]. [5] A.R. Brown and L. Susskind, Second law of quantum complexity, Phys. Rev. D 97 (2018) 086015 [arXiv:1701.01107] [INSPIRE]. [6] L. Susskind, Computational Complexity and Black Hole Horizons, Fortsch. Phys. 64 (2016) 24 [Addendum ibid. 64 (2016) 44] [arXiv:1402.5674] [INSPIRE]. [7] A.R. Brown, D.A. Roberts, L. Susskind, B. Swingle and Y. Zhao, Holographic Complexity Equals Bulk Action?, Phys. Rev. Lett. 116 (2016) 191301 [arXiv:1509.07876] [INSPIRE]. [8] A.R. Brown, D.A. Roberts, L. Susskind, B. Swingle and Y. Zhao, Complexity, action and black holes, Phys. Rev. D 93 (2016) 086006 [arXiv:1512.04993] [INSPIRE]. [9] R. Jefferson and R.C. Myers, Circuit complexity in quantum field theory, JHEP 10 (2017) 107 [arXiv:1707.08570] [INSPIRE]. [10] S. Chapman, M.P. Heller, H. Marrochio and F. Pastawski, Toward a Definition of Complexity for Quantum Field Theory States, Phys. Rev. Lett. 120 (2018) 121602 [arXiv:1707.08582] [INSPIRE]. [11] P. Caputa, N. Kundu, M. Miyaji, T. Takayanagi and K. Watanabe, Liouville Action as Path-Integral Complexity: From Continuous Tensor Networks to AdS/CFT, JHEP 11 (2017) 097 [arXiv:1706.07056] [INSPIRE]. [12] M. Moosa, Divergences in the rate of complexification, Phys. Rev. D 97 (2018) 106016 [arXiv:1712.07137] [INSPIRE]. Phys. Rev. D 90 (2014) 126007 [arXiv:1406.2678] [INSPIRE]. HJEP06(218) JHEP 01 (2016) 084 [arXiv:1509.09291] [INSPIRE]. JHEP 03 (2017) 118 [arXiv:1612.00433] [INSPIRE]. [arXiv:1501.01053] [INSPIRE]. [1] J.L.F. Barbon and E. Rabinovici , Holography of AdS vacuum bubbles , JHEP 04 ( 2010 ) 123 [2] J. Maldacena , Vacuum decay into Anti de Sitter space, arXiv: 1012 .0274 [INSPIRE]. [14] L. Susskind , The Typical-State Paradox: Diagnosing Horizons with Complexity, Fortsch . Phys. 64 ( 2016 ) 84 [arXiv: 1507 .02287] [INSPIRE]. [15] V.A. Belinski and I.M. Khalatnikov , Effect of Scalar and Vector Fields on the Nature of the Cosmological Singularity, Sov . Phys. JETP 36 ( 1973 ) 591 [INSPIRE]. [16] V.a. Belinsky , I.m. Khalatnikov and E.m. Lifshitz , A General Solution of the Einstein Equations with a Time Singularity, Adv . Phys. 31 ( 1982 ) 639 [INSPIRE]. [17] J.L.F. Barbon and E. Rabinovici , Holographic complexity and spacetime singularities, [18] L. Lehner , R.C. Myers , E. Poisson and R.D. Sorkin , Gravitational action with null boundaries , Phys. Rev. D 94 ( 2016 ) 084046 [arXiv: 1609 .00207] [INSPIRE]. [19] D. Carmi , R.C. Myers and P. Rath , Comments on Holographic Complexity, [20] A. Reynolds and S.F. Ross , Divergences in Holographic Complexity, Class. Quant. Grav. 34 ( 2017 ) 105004 [arXiv: 1612 .05439] [INSPIRE]. [21] K. Parattu , S. Chakraborty , B.R. Majhi and T. Padmanabhan , A Boundary Term for the Gravitational Action with Null Boundaries, Gen . Rel. Grav. 48 ( 2016 ) 94

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Stefano Bolognesi, Eliezer Rabinovici, Shubho R. Roy. On some universal features of the holographic quantum complexity of bulk singularities, Journal of High Energy Physics, 2018, 16, DOI: 10.1007/JHEP06(2018)016