Liouville mode in gauge/gravity duality

We establish solutions corresponding to AdS4\documentclass[12pt]{minimal} \usepackage{amsmath} \usepackage{wasysym} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{amsbsy} \usepackage{mathrsfs} \usepackage{upgreek} \setlength{\oddsidemargin}{-69pt} \begin{document}$$_4$$\end{document} static charged black holes with inhomogeneous two-dimensional horizon surfaces of constant curvature. Depending on the choice of the 2D constant curvature space, the metric potential of the internal geometry of the horizon satisfies the elliptic wave/elliptic Liouville equations. We calculate the charge diffusion and transport coefficients in the hydrodynamic limit of gauge/gravity duality and observe the exponential suppression in the diffusion coefficient and in the shear viscosity-per-entropy density ratio in the presence of an inhomogeneity on black hole horizons with planar, spherical, and hyperbolic geometry. We discuss the subtleties of the approach developed for a planar black hole with inhomogeneity distribution on the horizon surface in more detail and find, among others, a trial distribution function, which generates values of the shear viscosity-per-entropy density ratio falling within the experimentally relevant range. The solutions obtained are also extended to higher-dimensional AdS space. We observe two different DC conductivities in 4D and higher-dimensional effective strongly coupled dual media and formulate conditions under which the appropriate ratio of different conductivities is qualitatively the same as that observed in an anisotropic strongly coupled fluid. We briefly discuss ways of how the Liouville field could appear in condensed matter physics and outline prospects of further employing the gauge/gravity duality in CMP problems.


Introduction
This paper is motivated by recent progress in applying the AdS/CFT correspondence to condensed matter physics. Since several universal bounds (momentum η/s ≥ 1/4π and charge σ DC /χ ≥ d/4π T (d − 2) transport bound relations in holographic hydrodynamics [1][2][3][4], ω g /T c 8 in holographic superconductivity [5]) have been established for strongly coupled effective dual media, it is reasonable to pose the question: How robust are these relations? If one is limited to the standard gravitational theory setup no signs of violation of these universal bounds have been found. 1 However, different extensions of general relativity with higher order curvature terms revealed the violation of these universal relations (see, e.g., [7][8][9]). But still the question remains: may violations of the universal bounds of gauge/gravity duality be found within the Einstein theory? In fact, the positive answer to this question is known and it is related to introducing anisotropy [10][11][12][13][14] on the horizon surface in black hole (BH) solutions.
Indeed, the origin of universality in gauge/gravity duality is closely related to properties of black holes. In further discussion two observations will be important: 1. Thermodynamics of static charged black holes is fully managed by the (g tt , g rr ) parts of the metric 2 and depends on global geometry of the horizon surface, more precisely on its integral volume. 2. The transport coefficients are determined by the local geometry of the horizon surface, as well as by the g rr part of the metric, which determines the radial coordinate value of the horizon location.
On account of these facts it is easy to see that either the modifications in the (g tt , g rr ) parts of BH solutions due to the change of the bulk gravitational dynamics [7][8][9] (without changing the horizon geometry) or changing the horizon surface geometry to the anisotropic one [10][11][12][13][14] (without changing the standard dynamics of the bulk gravity) should lead to corrections to universal relations. Note, however, that the latter case requires introducing additional fields, as compared to the standard Einstein-Maxwell system. In this paper we will limit ourselves with the standard dynamics managed by the Einstein-Hilbert-Maxwell action and will take a look at universality in gauge/gravity duality from a different angle. It is clear from the discussion above that the universality violation will require changing in the horizon geometry. In [10][11][12][13][14] the standard geometry of the horizon surface was changed to the anisotropic one, modifying the planar geometry of the horizon with factoring one of the horizon coordinates by a function of the radial coordinate H(r ). By means of differential geometry it is easy to see that since such a deformation of the horizon is not isometric (it preserves the orthogonality of the coordinate system, but it does not preserve the volume of the horizon), it does not change the geometry type: the external curvature of the horizon surface is still equal to zero. Therefore, one may apply the same computational scheme to calculate the transport coefficients (the AC/DC conductivity and the shear viscosity [10,13,14]) as was done before [1,2,6]. Our proposal consists in performing another deformation of the horizon surface, which is also not isometric but still keeps the planar geometry: the horizon surfaces considered here are conformally flat. Unlike the deformation previously considered in [10,11], we consider "inhomogeneity" on the horizon surface encoded in function(s) solely dependent on the horizon surface coordinates. But we do it in a way which realises the conformal flatness of the horizon that in its turn justifies employing the technique of [1,2] in computing transport coefficients.
The rest of the paper is organised as follows. In Sect. 2 we formulate out setup, which is a standard one in searching for the solutions corresponding to charged black holes in 4D AdS space-time. Then, due to the two-dimensional surface theory, we can write down the part of the metric ansatz, corresponding to geometry of the horizon surface, in terms of isothermal coordinates. Recall that, written in the isothermal coordinates, any two-dimensional surface of genus zero possesses the geometry of conformally flat space. The log of the conformal factor in exponential parameterisation (the socalled metric potential) solely depends on the horizon surface coordinates. In the case of 2D constant curvature horizons the metric potential satisfies the elliptic Liouville equation. This is the way how the Liouville mode appears. We establish a general form of the Raissner-Nördstrom black hole solutions with electric and magnetic charges, the horizons of which have the planar, spherical and hyperbolic geometry. The Liouville mode of the solution carries the information on inhomogeneity on the horizon surface, which from the point of view of effective dual theory on the boundary of the AdS space plays the role of an inhomogeneity distribution function in a dual medium.
In Sect. 3 we calculate the charge diffusion coefficient and the DC conductivity on the inhomogeneous planar horizon of the electrically charged black hole within the stretched horizon approach [18] and the hydrodynamic limit of the AdS/CFT correspondence [1,2]. Here we derive the Fick law of diffusion in inhomogeneous media and observe the exponential suppression in the diffusion coefficient. The latter results in violation of the universal bound of [3] for suitable configurations of the metric potential. In Sect. 4 we extend our computations to the shear viscosity in the effective inhomogeneous fluid and establish the same bound value of η/s ratio as in [1,2]. However, fulfilment of this relation in the considered case reveals the exponential suppression of the KSS [1,2] bound value η/s 0 = 1/4π , computed for the trivial Liouville mode.
Section 5 contains our comments on the transport coefficients in the background of black holes with non-planar inhomogeneous horizons, on occurrence of the Liouville equation in models of condensed matter physics, and on generalisation of the obtained solutions to higher-dimensional AdS spaces.
In the latter case we observe two different conductivities on an inhomogeneous horizon of a 5D AdS electrically charged black hole. We establish conditions under which the ratio of different conductivities corresponding to [13] behaves qualitatively the same as for the strongly coupled anisotropic plasma model of [11,12]. In this section we also give an example of the Liouville mode configuration in the planar black hole solution, which preserves the KSS universal bound and fits the experimentally observed upper bound value of η/s ratio.
In the last section we present a summary of the results. For the reader's convenience, we add appendices containing the notation and useful information on solutions to the elliptic Liouville equation.
2 Raissner-Nördstrom black holes with inhomogeneity on the horizon surface

Setup
Let us consider the Reissner-Nördstom (RN)-type solution to the Einstein-Maxwell system in AdS space-time with cosmological constant , the dynamics of which is described by the following action (k 2 = 8π G): (2.1) Integration over M/∂M stands for the integration over the AdS/boundary manifold; h mn is the induced metric on the boundary in the r space-time foliation, n m = √ g rr δ mr is the outward normal to the boundary surface. We will find the RN-type solution to the Einstein-Maxwell equations of motion over the AdS 4 background with inhomogeneous horizon metric which generalises the planar (AdS) BH solution [15,16]. As usual = −3/l 2 , where l is a characteristic length of the AdS space.

Solutions for charged AdS BHs
To complete the task let us recall geometric properties of twodimensional surfaces, which lie at the basis of string theory. The line element of any two-dimensional surface of genus zero can be presented in the following way: where (x, y) are the isothermal coordinates (see, e.g., Chapter 9, Addendum I of [17]). A function (x, y) is often called the potential of the metric. On account of (2.5) we get the following BH solutions to the AdS 4 Einstein equation (2.3) with zero Maxwell field and constant curvature horizon manifolds 3 : • For a planar-type BH with (x, y) satisfying the elliptic wave equation • For a spherical type BH with (x, y) satisfying the elliptic Liouville equation • For a hyperbolic type BH 4 3 See Appendix A for details on the used notation. 4 In Schwarzschild coordinates the corresponding interval looks like with (x, y) satisfying the elliptic Liouville equation Recall that the Liouville equation Depending on the Gauss curvature of the horizon surface we choose K = 0, ±1; Q e,m are the values of the electric/magnetic charge densities. As for the neutral BHs, the metric potential (x, y) has to satisfy the elliptic Liouville equation (2.12). The Bianchi identities hold on the vector field ansatz (2.14).
Having established the solutions for the charged AdS BHs with inhomogeneous horizons, let us turn to computations of the related charge/momentum transport coefficients. From now on we will focus on the solution for electrically charged BH with the planar-type inhomogeneous horizon (i.e., on the solution (2.12)-(2.14) with K = 0 and Q m = 0).

Charge diffusion on a stretched horizon
A quick way to obtain the charge diffusion coefficient is to use the stretched horizon approach of [18] (see also [19][20][21] for early papers on electrodynamics of BHs and [22] and references therein for an introduction to the membrane paradigm approach).
It is a well-known fact (see, e.g., [6,18]) that the variation of the Maxwell action in a BH gravitational background fieldḡ mn leads to the boundary term at the BH horizon 5 r + , which is compensated for by the following surface term added to the action (cf. the action (2.1)): Hereh is the induced background metric on the stretched horizon r = r + + , 1 in the r space-time foliation, n m = √ḡ rr δ mr is the outward normal to the horizon surface, and j m is the conserved current induced on the horizon 6 Now we will treat the Maxwell field as a small perturbation over the gravitational background. In the linear order of perturbations the Einstein-Maxwell system (2.2)-(2.3) reduces to the AdS 4 Einstein equation R mn (ḡ) = ḡ mn , which is solved with (2.6)-(2.7), and to the Maxwell field equation of motion ∂ m ( √ −ḡF mn ) = 0 in the background ofḡ mn . The conformally flat structure of the horizon geometry makes possible to use the plane wave representation (see Section 3.7. in [23]) for the perturbed Maxwell field. Without loss of generality we can choose Calculations of the DC conductivity are performed at q → 0 (see [1,6]). The requirement of the Maxwell field regularity near the horizon imposes the following boundary condition [6]: The horizon is located at r = r + , where r + is the highest root of equation f (r ) = 0. 6 Indeed, Alternatively, this boundary condition follows from the solution to the Maxwell equations in the near-horizon limit [1]. Other assumptions lying in the basis of the charge diffusion law derivation and compatible with a q 2 /T 2 1 vector field series expansion (here T is the BH temperature) are [1] and Adapting the computational scheme of [1] to the considered case one may check the validity of (3.7) and (3.8).
and on account of (3.6) and (3.7) we derive Using the definition of (3.4a) we further get Finally, we obtain which is the covariantisation of Fick's first law for inhomogeneous media (compare to the corresponding expression in [1]). The diffusion coefficient entering (3.10) becomes a function of the horizon coordinates x, y where we have explicitly marked out the part depending on the x, y coordinates. Fick's second law comes from the current conservation: (3.12) The Ohm law contains the expression for the DC conductivity on the horizon: (3.14) From the Einstein relation D = σ DC /χ we can read off the charge susceptibility χ . 7 Now it is clear that the previously found universal relation receives corrections even in the case of the pure Einstein gravity setup. Indeed, in the considered case is exponentially suppressed. The violation of this bound strongly depends on the choice of inhomogeneity distribution function (x, y). 8 If the distribution function is positively valued in the selected domain, the damping strength is determined by the local inhomogeneity degree on the horizon surface.
Following the AdS/CFT prescriptions in computing the retarded Green's function, let us consider a small perturbation of the Maxwell field δ A m 1 over the RN background (3.16) 7 The Einstein relation can be deduced from the standard arguments [3].
The charge density at the AdS boundary r → ∞ can be computed from (3.4a) and the Maxwell field configuration δ A t (r ) = (μ − Q/r ) which satisfies the electrostatic Poisson equation with the boundary conditions δ A t (∞) = μ and δ A t (r + ) = 0. Then, at the leading order of ρ(T, μ) and μ(T ), ρ = e (x,y) Q = χμ, where μ is the chemical potential and χ is the charge susceptibility. Clearly,  ( (x, y)).
We choose an effective perturbation ansatz 9 : Then, in the leading order of perturbations, the vector field equation of motion (2.2) turns into Setting the effective perturbed field to the plane wave in the x direction (3.19) and plugging (3.19) back to (3.18) we conclude that the dynamical equations of the perturbed vector mode in the linear order approximation are compatible in the q → 0 limit. The dynamics of A x (r ) is determined by the last equation of (3.18): which we rewrite to The solution to the latter equation in the ω → 0 limit is apparent; it is 10 with some constant α. This constant is fixed by the requirement of having the in-falling boundary condition near the horizon (see, e.g., Appendix A of [6]): (3.23) 9 Obviously, we lose the symmetry in x, y directions with a general choice of the metric potential (x, y). So the correct ansatz for the Maxwell field perturbations (3.17) should also depend on y coordinate. However, we handle (3.19) as an effective perturbation, referring the reader to the next subsection, where we explain the relation between the general perturbation ansatz and what we call here the effective perturbation. 10 One may check is the solution to (3.20) satisfying the in-falling boundary condition in the near-horizon limit and the second boundary condition A x → 1 at r → ∞.
Comparing (3.22) to (3.23) in the near-horizon limit we get α = 1 √ −ḡ ttḡrr r . (3.24) According to the AdS/CFT recipe [26][27][28][29] we have to substitute the solution to the dynamical bulk equation into the boundary term (3.25) and to extract the retarded Green's function: Applying the Kubo formula of the linear response theory leads to the following expression of the DC conductivity near the horizon: which coincides with Eq. (3.14) obtained within the stretched horizon approach. The same arguments as before (see footnote 7 to this end) lead to the charge diffusion on the horizon with the coefficient so we arrive at the same conclusions on violation of the KR [3] universal bound as in the previous subsection.

"R-charge" diffusion pole
To verify (3.15) and (3.28) we will directly obtain the charge diffusion coefficient adapting the computational scheme of [1,25] to the considered case. Because we are aimed at calculation of the diffusion coefficient from the pole of Green's function in the momentum representation both temporal and spatial components of a four momentum have to be nontrivial. Following [1,25] we consider the Maxwell equation on a background defined by ds 2 = g tt (r )dt 2 + g rr (r )dr 2 +(g x x (x, y)dx 2 + g yy (x, y)dy 2 ). (3.30) We will suppose that g x x = g yy = r 2 f (x, y) and √ −gg x x , √ −gg yy are constants. After fixing the gauge A r = 0 and requiring the most general form of the Maxwell field Here the prime denotes the differentiation over r .
The system of Eqs. (3.32)-(3.35) does not in general admit a decoupled vector field mode. However, we can further specify the ansatz for the Maxwell field to set q (y) A x = q (x) A y . Then Eqs. (3.32)-(3.35) turn into where we have introduced the effective metric in the x, y directions The structure of (3.36)-(3.38) is similar to the corresponding system of equations of [1] (or [25]), the solution to which leads to the expression for the charge diffusion coefficient. Following [1,25], let us join (3.36), (3.37) into a single equation, d dr On account of (3.36), Eqs. (3.37) and (3.38) become equivalent, so it is enough to solve (3.40) for A t . Now we specify the background metric (see (2.6)): (3.41) Searching for solutions to the second order w.r.t. A t Eq. (3.40) is simplified with introducing new radial variable u = r + /r . Setting l = r + = 1 and ω 2 M/r + = 1, the gravitational background becomes The metric potential (x, y) still obeys the elliptic wave equation (2.7); the set of expressions (3.41) turns into and where the prime now corresponds to the derivative over u. It is also convenient to turn to the rescaled momentumq 2 = γ q 2 (x) = q 2 (x) + q 2 (y) and to introduce the dimensionless energy and momentum, Equation (3.44) is perturbatively solved in the small w, q 2 approximation [1,25] with the following ansatz: The overall constant C of (3.46) is fixed from Eq. (3.37) written in u variable (3.49) Taking the limit u → 0 we get , (3.50) and the pole in C is the diffusion pole with the diffusion "constant" In the case of a perturbation of the Maxwell mode over the RN background

52)
the solution to (3.44) may be found [30] from that after the same steps as before leads to the diffusion pole at iw = e − q 2 /(1 − k 2 Q 2 /6). On account of the relation between the Hawking temperatures of the RN and neutral BHs we end up with the diffusion coefficient Comparing the values of the charge diffusion coefficients (3.51), (3.56) to that of previously obtained from the membrane paradigm (Eq. (3.15)) and from the effective Maxwell field perturbations ansatz (Eq. (3.28)) we note that the results coincide. A formal correspondence between variables in the former and in the latter computing schemes is as follows: Note also that the dispersion relation, following from the second Fick law (3.12), contains the term linear in the momentum with the gradient of the metric potential (x, y). This contribution to the diffusion pole has to appear after relaxing the imposed condition q (y) A x = q (x) A y . Such a generalisation for the Maxwell field perturbation is beyond the scope of the paper and will be done elsewhere. Below we will see the appearance of the linear over momentum term in the diffusion pole of gravitational perturbations over AdS 4 BH background.

Shear viscosity and η/s ratio
In this part of the paper we compute the η/s ratio for the planar BH solution with inhomogeneous horizon surface. As in the previously considered case of charge diffusion, calculations in this section are divided into two parts. We perform quick effective computations first, after that we will turn to a more rigorous computational scheme to verify the result.
Expanding the Einstein equation R mn = g mn to the linear order in the fluctuations we get , where we have used Eq. (2.7). Taking one may notice that the resulted system of equations is compatible to the zero momentum limit q → 0, which is suitable for our aims. Therefore, to compute the shear viscosity we have to solve the equation for h xy (r ) first. Plugging (4.2) into the x y part of the perturbed Einstein equation one gets which on account of the explicit expression for f (r ) can be written down in the following form: Then the resulting equation for h xy coincides with that obtained in [31] Again, the constant α is fixed by the in-falling boundary condition at the horizon Comparing (4.6) to (4.7) in the near-horizon limit results in with the entropy density Here we have denoted the entropy of a BH with isotropic homogeneous horizon s 0 . Clearly, the entropy density s becomes a function of the local distribution (x, y). The on-shell action for the perturbed gravity mode is as follows: Plugging the retarded Green function into the Kubo formula leads to the well-known expression [25] η/s = 1 4π . (4.12) Now, once we recover the KSS η/s 0 ratio [1], from (4.9) we get ,y) . (4.13) Therefore, as in the case of charge diffusion near the BH inhomogeneous horizon, the KSS universal bound relation η/s 0 ≥ 1/4π receives exponential suppression. The range of its violation and the possibility to violate this bound at all strongly depend on the local properties of the metric potential (x, y) (see the discussion around footnote 8). Equation (4.13) also follows from computations of the shear viscosity in the RN background metric (3.16) or its magnetically charged cousins (solutions (2.13)-(2.14) with K = 0).

Diffusion pole in 4D AdS BH with Liouville mode
Now we will check the relation (4.13) by computing the shear viscosity from the diffusion pole of gravitational perturbation Green's function [1,25]. It is convenient to turn to the AdS 4 BH background in u radial variable to this end: (4.14) Equation (4.14) defines the background metricḡ mn , and we choose the perturbation of the gravitational field g mn = g mn + h mn , h mn 1 in the following form: with the other components of h mn equal to zero (we work in the h mu = 0 gauge). Imposing the elliptic wave equation on the metric potential (x, y), we get the following equations for the non-trivial components of h mn up to the second order in perturbations: Equations (4.16)-(4.18) are consistent once ∂ y h ty = 0, ∂ y h xy = 0 and ∂ y = 0. The consistency conditions select "chiral" in x, y plane modes with h mn = {h ty (t, u, x)/u 2 , h xy (t, u, x)/u 2 } and (x, y) → (x). However, the "chirality" condition on the metric potential is stringent enough: together with the elliptic wave equation it narrows the choice of non-trivial metric potential to (x) = αx + β. Hence, we have to relax ∂ y (x, y) = 0. To relax the "chirality" condition on the metric potential (x, y) we add other "chiral" perturbation modes in y direction, H mn = {H t x (t, u, y)/u 2 , H xy (t, u, y)/u 2 }, H mn 1. As a result we have the following system of non-trivial equations for the perturbed metric g mn =ḡ mn + h mn + H mn in the first order in the perturbations: while the tt, tu, uu components of the AdS 4 Einstein equation turn to identities. Additionally we have the following consequences of the x x and yy components of the AdS 4 Einstein equation: (4.26) Turning to the Fourier modes H mn (t, u, y) = dω (y) dq (y) (2π) 2 e −iω (y) t+iq (y) y H mn (ω (y) , q (y) , u), (4.27) one may check that the consistency of (4.25) with (4.22)-(4.24) requires Equations (4.26) in the momentum representation are  (4.23), (4.24) are (on account of (4.22)) solutions to (4.25).
Here d (y) = 3∂ y /(4π T ) and w (y) = 3ω (y) /(4π T ), q (y) = 3q (y) /(4π T ). Substituting the ansatz (4.33) in (4.31) we get The constant C is fixed from the original equation (4.23) at the boundary of AdS space (4.36) Therefore, the diffusion coefficient in y direction is equal to Since D = η/( + P) and + P = s 0 T , 11 Equation (4.32) solves in the same way, so the diffusion coefficient in x directions is also defined by (4.37). Therefore, Eq. (4.13) holds. We pay the reader's attention on the occurrence of linear in the corresponding momentum term in the diffusion poles of gravitational perturbations along x, y directions. As we have pointed out above, this term results from the diffusion law in inhomogeneous media (see Eq. (3.58)).

Comments on transport coefficients for non-planar inhomogeneous horizons
Calculations performed in previous sections may be extended to the case of black hole solutions with non-zero constant curvature horizons (solutions (2.13)-(2.14) with K = ±1).
In this cases one also gets the exponential suppression in formulae for the diffusion coefficient and for the η/s 0 ratio, Eqs. (3.15) and (4.13). Formally the results are the same; however, there are differences in compare to the case of a planar inhomogeneous horizon. Looking at solutions to the elliptic Liouville equation (some of which are borrowed from [33] and presented in Appendix B), one can notice that exp(± (x, y)) contains in general different singularities: poles of complex functions entering the solution for the spherical-type horizon and zeros of their derivatives/specific combination (cf. Crowdy's solution (B.8)), or simultaneous zeros of a function derivatives in x, y directions/zeros of functions (cf. Popov's solution (B.9) [34]) for the hyperbolic-type horizon. These obstacles should be taken into account upon the choice of trial functions for 11 Thermodynamic equilibrium is defined by 0 + P 0 = s 0 T 0 at zero metric potential. Turning the metric potential on one gets e − ( 0 + P 0 ) = s 0 e − T 0 , that is, + P = s 0 T . the Liouville mode: various singularities of functions and their derivatives have to be avoided to keep a well-defined range of physically accepted values of γ i j components of the metric tensor and their inverse. Note that in both cases (with K = ±1) exp (− (x, y)) takes the whole range of values (smaller and greater than one), hence the exponential suppression of D and η/s 0 with violation of the universal bounds takes place within the local domains of exp(− (x, y)) < 1.

Comments on the Liouville field in condensed matter physics
The Liouville equation has been widely recognised in 2D QFT (see, e.g., [35,36] for comprehensive reviews). On the condensed matter physics side the appearance of the Liouville field theory may be found in the description of disordered charged media at the strong coupling limit [37] and in the consideration of particle motion in a random potential [38] or in a diffusion process of a random walk particle in the δ-potential [39,40] (see also [41] for a review of diffusion processes in disordered media). These observations give us evidence to interpret the parameter of inhomogeneity of the horizon (x, y) as the inhomogeneity degree in the dual strongly coupled effective media related to its disorder and the degree of chaotisation. We hope it opens a new prospect in searching for a holographic description of such CMP models in terms of the gauge/gravity duality. 12

Comments on higher-dimensional generalisation of the solutions
Higher-dimensional generalisation of the solutions (2.13)-(2.14) is easy to derive on account of the previously found solution for an electrically charged AdS n+1 black hole [47]. Adapting to our case this solution transforms into where the metric potential (x, y) satisfies the elliptic Liouville equation Applying the technique has been used in computing transport coefficients, one may found the effect of anisotropy in n-dimensional effective dual media. For instance, in 5D case we get two different conductivities: σ x x = σ yy = r + , σ zz = r + e , (5.3) and two different diffusion coefficients: one of which is at the KR [3] bound value; the other one is exponentially suppressed. The ratio σ zz /σ x x = e depends on the degree of inhomogeneity, determined by the metric potential, and it is always smaller than one inside domains of exp( (x, y)) < 1, where the KR bound holds. Similar behaviour of σ zz /σ x x = 1/H(r ) was early established in the strongly coupled anisotropic plasma [10][11][12][13][14] with the anisotropy function H(r ), so we observe the formal correspondence exp(− (x, y)) H(r ) between the (inverse of) inhomogeneity distribution function on isotropic horizon and the anisotropy function of a homogeneous horizon surface. 13

Fitting to RHIC and LHC data
The combined analysis of all data of high-ion collisions measured at RHIC and at LHC gives the following experimental restrictions on the η/s value [45,46]: η/s ∼ 0.12 (RHIC), η/s ∼ 0.2 (LHC). (5.5) In the following we will focus on the LHC result. Also we will accept the KSS value for the lower bound, η/s 0 ∼ 0.08. According to our calculations, the η/s ratio, measured in s 0 units, is not a constant anymore; it is a function of the Liouville mode (x, y) (cf. (4.13)) with natural "boundary condition" η Hence, in our interpretation a wide range of experimentally fixed values of η/s (5.5) is an impact of the local inhomogeneity distribution in quark-gluon plasma. Then the KSS bound value corresponds to the QGP near-equilibrium isotropic homogeneous state. Now our aim is to find a shape of the metric potential (x, y) which will satisfy: (1) the Liouville equation; and (2) the b.c. (5.6) and the upper value bound η/s ∼ 0.2. From the discussion in Sect. 5.1. we have only a chance to realise the experimentally estimated upper bound value with (x, y) unbounded from below and having the upper bound to be equal to zero. The simplest way to realise the required shape of (x, y) is to consider the planar-type BH horizon surface, so the metric potential has to satisfy the elliptic wave equation (2.7).
By trials and errors method we found the following trial form of (x, y), which falls within the above-mentioned criteria: To satisfy the upper bound η/s 0.2, the BH horizon should be restricted in x, y directions to x ∈ [−0.9 + 2 √ 2 π, 2 √ 2 π ], y ∈ [− √ 2, √ 2] (see Fig. 1). Then, depending on the local value of the true inhomogeneity distribution density on the BH horizon surface exp( (x, y)), 14 one recovers the whole range of theoretical and experimental values 0.08 ≤ η/s ≤ 0.2 with the entropy density s measured in units of s 0 . This example illustrates advantages of the developed approach, when having unfixed functions converts fitting to experimental data into a merely technical task.

Summary and conclusions
To summarise, we have obtained solutions to the Einstein-Maxwell dynamical system, which correspond to the static charged AdS black holes with inhomogeneity distribution function on the black hole horizon surface. The inhomogeneity of 2D horizon surface is encoded in the conformal factor entering the metric ansatz, which depends on the horizon coordinates and whose dynamics obeys the Liouville equation. That is why we have called such ingredient of the metric as the Liouville mode.
Focusing on the AdS 4 space-time we have computed the charge diffusion coefficient and the DC conductivity on the horizon within the stretched horizon approach and have observed that: 1. The resulting Fick's laws describe diffusion in inhomogeneous strongly coupled dual media, which is natural to expect. 2. The diffusion coefficient is exponentially suppressed, which may in principle violate the previously suggested KR universal bound for the diffusion constant [3]. In all possible cases the violation degree is proportional to the strength of the local inhomogeneity.
We have also calculated the charge diffusion and transport coefficients in the hydrodynamic limit of AdS/CFT correspondence and have realised that the KSS shear viscosity-perentropy density universal bound [1,2] is also exponentially suppressed. Hence, we have observed the violation of the KSS/KR universal bounds in backgrounds of charged black holes with planar/spherical/hyperbolic horizons within the standard Einstein-Maxwell setup. In all these cases we have observed that the violation of universal bounds depends on the explicit choice of the inhomogeneity distribution on the horizon and may be in general realised in local domains of its positivity. To show the relevance of the approach in situation when universal bounds hold we have given an example of the inhomogeneity distribution function, which preserves the KSS η/s 0 ∼ 0.08 universal bound and fits all the range of experimentally measured at RHIC and at the LHC values of η/s ratio in s 0 units.
The extension of the obtained solutions for RN black holes with constant curvature inhomogeneous horizons to higherdimensional AdS spaces revealed the appearance of two different conductivities in 4D effective charged dual media, the corresponding ratio of which, within domains of preserving the KSS/KR bounds, possesses the same qualitative feature as that of previously found in 4D anisotropic strongly coupled plasma [13].
Turning back to occurrence of the Liouville equation in condensed matter physics problems, we recall that the Liouville field theory naturally appears in CMP models related to diffusion processes in random media, or to the description of strongly coupled disordered media [37][38][39][40]. We believe that our results open a new prospect in searching for holographic description of physical processes in disordered media at the strong coupling constant regime. We hope to report on progress in this and other directions in the future.