# Hysteresis in for QFTs dual to spherical black holes

###### Abstract

We define and compute the (analogue) shear viscosity to entropy density ratio for the QFTs dual to spherical AdS black holes both in Einstein and Gauss-Bonnet gravity in five spacetime dimensions. Although in this case, owing to the lack of translational symmetry of the background, does not have the usual hydrodynamic meaning, it can be still interpreted as the rate of entropy production due to a strain. At large and small temperatures, it is found that is a monotonic increasing function of the temperature. In particular, at large temperatures it approaches a constant value, whereas, at small temperatures, when the black hole has a regular, stable extremal limit, goes to zero with scaling law behaviour. Whenever the phase diagram of the black hole has a Van der Waals-like behaviour, i.e. it is characterised by the presence of two stable states (small and large black holes) connected by a meta-stable region (intermediate black holes), the system evolution must occur through the meta-stable region and temperature-dependent hysteresis of is generated by non-equilibrium thermodynamics.

^{†}

^{†}journal: Eur. Phys. J. C

∎

e1mariano.cadoni@ca.infn.it \thankstexte2edgardo.franzin@ca.infn.it \thankstexte3matteo.tuveri@ca.infn.it

## 1 Introduction

In recent times, many efforts have been devoted to the investigation of the low-frequency, hydrodynamic limit of quantum field theories (QFTs) with holographic gravitational duals in the AdS/CFT framework. This hydrodynamic limit is a powerful tool to compute transport coefficients for strongly coupled QFTs, e.g. the quark-gluon plasma phase of QCD. In the hydrodynamic regime of thermal QFTs with gravitational duals, the shear viscosity to entropy density ratio is of particular interest. In fact, this ratio takes the universal value for all QFTs with Einstein gravity duals Policastro:2001yc (); Buchel:2004qq (); Benincasa:2006fu (); Kats:2007mq (); Landsteiner:2007bd (); Iqbal:2008by (); Buchbinder:2008nf (); Edalati:2009bi (). This has led to conjecture the existence of a fundamental lower bound — the Kovtun-Son-Starinets (KSS) bound Kovtun:2003wp () — which is supported both by energy-time uncertainty principle arguments and by quark-gluon plasma experimental data Kovtun:2003wp (); Kovtun:2004de (); Song:2010mg ().

In the usual setting of the AdS/CFT correspondence, the holographic dualities are utilised
to learn about transport coefficients in the hydrodynamic limit of strongly
coupled QFTs by investigating bulk gravity configurations, typically black branes.
However, this paradigm can be reversed and the properties of the dual QFT can be used
to infer about the behaviour of bulk gravity solutions.^{1}^{1}1For instance, this approach has been particularly
fruitful for the computation of the microscopic entropy of black holes.
In several cases, the Bekenstein-Hawking entropy has been matched
by counting states in the dual CFT — see e.g. Refs. Strominger:1996sh (); Cadoni:1998sg ().
In this perspective, transport coefficients computed in the hydrodynamic limit
of the dual QFT can lead to a deeper understanding of black hole (BH) physics.
In particular, the aim of this paper is to better understand the rich thermodynamical phase
structure of AdS BHs with spherical horizons (characterised by meta-stabilities and
Van der Walls-like behaviour Chamblin:1999tk (); Chamblin:1999hg (); Cvetic:2001bk ()) by
investigating the relationship between the shear viscosity of the dual QFT and the
thermodynamics of these BHs.

It is well-known that the KSS bound can be violated by two different kinds of effects: higher-curvature terms in the Einstein-Hilbert action Brigante:2007nu (); Brigante:2008gz (); Ge:2009ac (); Ge:2009eh (); Cai:2009zv (); Camanho:2010ru (); Cremonini:2011iq (); Jacobson:2011dz (); Bhattacharyya:2014wfa (); Sadeghi:2015vaa (); Wang:2016vmm (); Cadoni:2016hhd () and breaking of the translational or rotational symmetry of the black brane background Erdmenger:2010xm (); Erdmenger:2011tj (); Rebhan:2011vd (); Mamo:2012sy (); Davison:2015taa (); Hartnoll:2016tri (); Burikham:2016roo (); Alberte:2016xja (); Cadoni:2016hhd (); Liu:2016njg (). These two effects were the motivation to consider spherical AdS BHs, for which the translational symmetry is intrinsically broken, both in general relativity (GR) and in a higher-curvature theory, namely Gauss-Bonnet (GB) gravity.

The violation of the KSS bound in higher-curvature gravity theories, although not completely understood, can be traced back to finite-, finite- effects and to the inequality of the two central charges of the dual QFT Buchel:2004di (); Buchel:2008vz (). This lends support to the possibility of formulating modified bounds on , based for instance on causality and positivity of energy in the dual QFT Brigante:2008gz (); Buchel:2009tt (); Hofman:2009ug ().

On the other hand, the violation of the KSS bound due to the breaking of the translational symmetry has a more fundamental nature. In this case, the shear viscosity does not have the usual hydrodynamic meaning but might be interpreted as the rate of entropy production due to a strain Hartnoll:2016tri (); Davison:2015taa (); Rebhan:2011vd (); Mamo:2012sy (); Burikham:2016roo (); Romatschke:2009kr (). In this framework, the behaviour of as a function of the temperature is non-trivial Cremonini:2012ny (); Cremonini:2011ej () and carries information about the infrared (IR) and ultraviolet (UV) behaviour of the QFT, the existence of global diffusive modes of the system and the nature of the effect responsible for the breaking of translational invariance. For instance, when this breaking is generated by the presence of a non-homogeneous scalar field in the bulk, the behaviour of at small is determined by the flow of the QFT in the IR. If the translational invariance is restored in the IR then goes to a constant as , signalising the presence of an IR collective diffusive mode. Conversely, if the translational invariance is not restored, scales as for and the IR geometry in dimensions is typically Hartnoll:2016tri (). We will discuss the general validity of this behaviour for spherical BH backgrounds. In this case, the translational symmetry is intrinsically broken and cannot be restored in the IR, but holds only in the UV, where the spherical horizon can be approximated by a plane.

In a recent letter Cadoni:2017fnd (), a definition of the shear viscosity for QFTs living in manifolds whose spatial sections are spheres is proposed. This has allowed us to compute the spherical analogue of the shear viscosity for QFTs dual to five-dimensional AdS-Reissner-Nordström (AdS-RN) BHs in GR. Here, a detailed derivation of these results is presented and the discussion to five-dimensional asymptotically AdS neutral and charged BHs in GB gravity is extended.

We start by defining the (analogue) shear viscosity for a QFT living on a -sphere in the hydrodynamic limit. Although the shear viscosity does not have the usual interpretation pertaining to a QFT in a translation-invariant background, it is shown that it still satisfies a Kubo formula and can be interpreted in terms of entropy production due to a strain.

For a given tensorial perturbation of the spherical background it is possible to define three different correlators corresponding to shear, sound and transverse propagating modes Brigante:2007nu (). If all the background symmetries are unbroken they lead to the same value of the shear viscosity. If this is not the case, in general the value of becomes channel dependent Ciobanu:2017fef (). Therefore, in the case under consideration there will be three different determinations of the viscosity for shear, sound and transverse modes. In this paper the focus will be only on the shear viscosity for transverse perturbations, for which computations are easier.

Following the approach of Refs. Hartnoll:2016tri (); Lucas:2015vna (), we compute for QFTs dual to five-dimensional asymptotically AdS neutral and charged BHs in GR and GB gravity. By considering linear perturbations of the field equations, the computation of is reduced to the determination of the non-normalisable mode of the perturbation evaluated at the horizon. The perturbation satisfies a linear second-order differential equation analogous to a massive scalar equation in a curved background whose non-vanishing mass term encodes the breaking of the translational invariance. Whereas the large and small behaviours of are determined analytically, its global behaviour is determined numerically. It is shown that for certain regimes of the temperature is a monotonic function. It saturates the KSS bound at large (or the GB coupling constant dependent bound in the GB case), where the translational invariance is restored. When the BH has a regular, stable extremal limit goes to zero with a scaling law at small temperatures.

An interesting and somehow unexpected behaviour of emerges in the parameter regions where the BH has a Van der Walls-like behaviour, characterised by the presence of both a second and a first order phase transition. Once the control parameter (the GB coupling constant or the BH charge) falls below a critical value, the system undergoes a second order phase transition. In this condition, BHs may undergo a first-order phase transition from small to large BHs controlled by the temperature. Small and large black holes are connected through a meta-stable intermediate region. As a result, it is found that exhibits a temperature-dependent hysteresis and, close to the phase transition, it becomes multi-valued as expected for a first-order phase transition Erdmenger:2010xm (). We further explain this behaviour in terms of the non-equilibrium thermodynamics underlying the Van der Walls-like phase portrait.

The structure of the paper is as follows. In Sect. 2 we discuss the problems related to the hydrodynamic limit for QFTs dual to spherical BHs, the definition and the computation of and we derive the Kubo formula for . In Sect. 3 we review known facts about solutions, thermodynamics, phase structure and perturbations for AdS spherical BHs in GR and GB gravity. In Sect. 4 we give the general formula for , compute its large and small behaviours, give the numerical results for its global behaviour and discuss its relationship with the thermodynamical phase portrait of the dual BH solutions. Finally, in Sect. 5 we state our conclusions.

Throughout this paper indices refer either to the whole -dimensional bulk spacetime or to its -dimensional conformal boundary, while refer to the transverse -dimensional spatial sections.

## 2 Hydrodynamic limit for QFTs dual to spherical black holes and the analogue viscosity

Relativistic hydrodynamics is an effective long-distance description for a classical or quantum many-body system at non-zero temperature. In particular, it can be used to describe the non-equilibrium real-time macroscopic slow evolution of the system, both in space and time, with respect to a certain microscopic scale.

In the holographic framework of the AdS/CFT correspondence, the QFT lives in the boundary of a certain gravitational bulk region. In some cases, the QFT can be described by a kinetic theory and the microscopic scale is determined by the mean free path of particles and the typical momentum scale of the process . When the kinetic theory is absent or unknown, it is still possible to give a thermal description and interpret the inverse temperature as the microscopic scale Baier:2007ix (); Kovtun:2012rj (). Thus, the hydrodynamic limit of a QFT corresponds to large relaxation time, i.e. small frequencies, and large scales compared to the typical one of the system, i.e. , where is the wavelength of the excitations of the system.

In general, the existence of a hydrodynamic description is essentially due to the presence of conserved quantities, i.e. to the isometries of the system, whose densities can evolve (oscillate or relax to equilibrium) at arbitrarily long times provided the fluctuations are of large spatial size. Correspondingly, the expectation values of such densities are the hydrodynamic fields. However, it is still possible to give a hydrodynamic description of a system without conserved quantities in terms of expansion in derivatives of hydrodynamic fields (as the fluid velocity) Baier:2007ix (). This approach is followed to formulate the hydrodynamic description of a fluid in a spherical background holographically dual to AdS spherical BHs.

On the sphere, due to its intrinsic geometry, the translational invariance is broken. As a consequence, the momentum is not conserved and it is not possible to define an associated conserved current. At first sight, this should prevent us from studying transport coefficients as the shear viscosity which is, by definition, a measure of the momentum diffusivity due to a strain in a fluid. Hence, in principle, without translational symmetry it is not possible to define a conserved current, from which the Fick law of diffusion Son:2007vk () can be derived. Nevertheless, as seen below, these difficulties can be circumvented and a rigorous definition of for the hydrodynamic limit of a QFT in a spatial background without translational isometries can be given.

Consider a QFT living on the boundary of whose spatial sections have spherical topology. Although bulk BHs allow for dual QFTs living on a sphere Gubser:1998bc (); Witten:1998qj (); Cho:2002hq (); Neupane:2009zz (), the explicit form of the holographically dual QFT is not of interest here. However, its hydrodynamic limit can be studied in the sense described above. The boundary metric is conformal to

(1) |

where is the metric of a -sphere. In this case, due to the spherical shape of the boundary, the metric perturbations used to describe the non-equilibrium real-time macroscopic slow evolution of the system are characterised by two parameters, the relaxation time or the frequency and which “measures” angular distances on the sphere. The integer number parametrises the eigenvalue of the Lichnerowicz operator on the sphere (see Eq. 7 below) and is analogous to the momentum scale for a flat topology. In the spacetime (1), the hydrodynamic limit of the holographic QFT is defined as the limit in which the metric perturbations have slow relaxation time and are much larger than the typical scale of the system, i.e. and . Since we are dealing with a -sphere, the number cannot be arbitrarily small, i.e. there is a minimum value Kodama:2003jz (); Ishibashi:2003ap (); Gibbons:2002pq () which corresponds to a maximum spatial scale, and to a maximum size for the global modes propagating on the sphere. On the contrary, in flat space, there is no constraint on the values of . Thus, one can set which corresponds to fluctuations of very large (in principle infinite) wavelength.

### 2.1 Hydrodynamics in curved spacetime

Relativistic hydrodynamics for a fluid in curved spacetimes can be formulated starting from the following definition for the stress-energy tensor Romatschke:2009kr (); Baier:2007ix ()

(2) |

where is the energy density and the fluid velocity (commonly evaluated in the frame in which the fluid is at rest) is timelike. The tensor is the spatial part of the stress-energy tensor and it is made by time-independent functions of the hydrodynamic variables , and their derivatives. In a generic curved background, it is not always possible to define globally conserved currents associated with symmetries of the system. However, the hydrodynamic equations can always be derived by requiring the stress-energy tensor to be covariantly conserved, i.e. . In general, the hydrodynamic modes are infinitely slower than all other modes and the latter can be integrated out. Thus, all quantities appearing in the hydrodynamic equations are averaged over these fast modes and are functions of the slow-varying hydrodynamic variables.

Equation 2 can be expanded in powers of derivatives of the velocity, and at first order, the most general expansion is given by

(3) |

where is a scalar function and it can be interpreted as the
thermodynamical pressure. The tensor contains the derivatives of the
fluid velocities, i.e. the dissipative contributions to . Its explicit
form is given by Romatschke:2009kr (); Baier:2007ix ()^{2}^{2}2For a rank-2 tensor,
,
where is a symmetric and transverse tensor given by
. In the local rest frame,
it is the projector tensor on the spatial subspace.

(4) |

where the dots represent the non-linear terms in the fluid velocity and , are transport coefficients. The symbol represents the derivative with respect to the velocity direction, i.e. . The tensor is a symmetric, transverse and traceless tensor constructed with the first derivative in the fluid velocity given by . The parameter is the shear viscosity and is the relaxation time.

### 2.2 Kubo formulas and the analogue viscosity

The Kubo formula relates thermal correlators to kinetic coefficients such as dissipative ones. For a relativistic QFT in flat spacetime, the Kubo formula gives a general definition of the shear viscosity in terms of the retarded Green function for the stress-energy tensor Kovtun:2004de (); Policastro:2002se (); Hartnoll:2016tri ()

(5) |

where , are the spatial components of the stress-energy tensor, and are the frequency and wave vector of the perturbation. When the translational invariance is preserved and a hydrodynamic limit exists, Eq. 5 becomes the Kubo formula for the transverse momentum. In this case, defined by Eq. 5 coincides with the usual hydrodynamical definition in terms of conserved quantities obtained from the Einstein relation , where is the diffusion constant appearing in the Fick law Hartnoll:2016tri (). In a holographic setup based on the AdS/CFT correspondence, can be calculated using the usual AdS/CFT rules by considering small perturbations of the bulk metric.

In order to extend the Kubo formula (5) to spherical backgrounds, small metric perturbations around the boundary background metric (1) are considerd, i.e. . In general, three different types of perturbations can be considered: shear, sound and transverse (scalar) modes. The behaviour of these modes will be encoded in three different correlators . In the translationally invariant case (and also when translation invariance is broken by external matter fields) at these three functions are equal, owing to rotational symmetry Brigante:2007nu (). By contrast, in the spherical case under consideration cannot be taken to zero by construction and the correlators will be different. Thus, in general, any definition of the shear viscosity in a spherical background based on linear response to small disturbances will be channel-dependent. In this paper the focus will be on the transverse perturbations. The computations for the sound and shear channel is left for future investigations.

Choosing transverse and traceless perturbations with if , (where denote the angular directions) in Eq. 3 and considering the fluid at rest, i.e. , we obtain

(6) |

where is the Lichnerowicz operator and it corresponds to a generalisation of the Laplacian for the -sphere, with . Equation 6 is analogous to the one obtained in Ref. Baier:2007ix () for planar topology. As required by linear response theory, the retarded Green function for the tensor channel is computed by choosing a harmonic time dependence for the perturbation, and by expanding in hyper-spherical harmonics Rubin:1983be (); Rubin:1984tc (); Higuchi:1986wu (), the retarded Green function can be extracted from Eq. 6,

(7) |

where are the eigenvalues of the Lichnerowicz operator and is an integer associated with the hyper-spherical harmonic expansion. The eigenvalues are positive and form a discrete set Higuchi:1986wu (); Kodama:2003jz (); Ishibashi:2003ap (); Gibbons:2002pq (). Given the retarded Green function above, the dissipative coefficients and can be extracted. In particular, the analogue of shear viscosity in the hydrodynamic limit for a QFT in a spatial spherical background in the transverse channel can be defined as,

(8) |

where is the minimum value of . Notice that the shear viscosity in Eq. 8 is defined as the limit of the retarded Green function in analogy with Eq. 5. In planar hydrodynamics, the limit describes long wavelength modes and probes large scales on the plane. In the spherical case, the modes probe large angles on the sphere.

It is also important to stress that, with respect to the planar case, the expression in square brackets in Eq. 6 has an additional contribution to the stress-energy tensor ruled by the transport coefficient . However this contribution drops out in the Kubo formula (8), when we take the imaginary part of the Green function.

We conclude with some remarks about the conservation of the stress-energy tensor. For translation-invariant backgrounds, the conservation of the stress-energy tensor leads to the conservation of global currents and to the Fick law Son:2007vk (). More generally, from the projection of along the fluid velocity , second-order hydrodynamics can be related with the second law of thermodynamics Baier:2007ix (). In particular, by using Eqs. 4 and 3 at linear order the following can be found

(9) |

where is the entropy density. Equation 9 represents the rate of entropy production in a fluid due to a slowly varying strain and it can be used to define the shear viscosity Hartnoll:2016tri ().

## 3 Black-hole solutions in five dimensions

The field equations of five-dimensional Einstein-Gauss-Bonnet gravity sourced by any form of matter fields described by the stress-energy tensor are Myers:1988ze (); Cai:2001dz (); Cai:2003kt ()

(10) |

where is the Einstein tensor, is the GB coupling constant, is the five-dimensional Newton constant, and is the GB contribution,

(11) |

For later convenience we define , being the AdS length. Throughout this paper, the source term contains only a negative cosmological constant and an electromagnetic field. In particular, we consider static BH solutions to (10) i.e. solutions with spherical horizons in the form

(12) |

For the AdS-RN BHs of GR the metric function is

(13) |

while, in the branch that allows for BH solutions, the metric function for GB gravity is

(14) |

In Sects. 3 and 13, and are, respectively, the BH mass and charge.

### 3.1 Black holes in Gauss-Bonnet gravity

As in the black brane case, asymptotically AdS BH solutions of GB gravity exist only for . Moreover, it is well-known that the unitarity bounds for the dual QFT constrain the value of Brigante:2007nu (); Ge:2008ni (); Ge:2009eh (), so that in this paper we will take in the following range .

The BH horizons are determined by the positive zeroes of the function

(15) |

where . The BH becomes extremal when .

Asymptotically AdS BH solutions with inner () and outer () horizons exist for

(16) |

where is the real, positive solution of the cubic equation . When the inequality is saturated, the inner and outer horizons merge, i.e. the BH becomes extremal and in the near-horizon regime the solution factorises as

(17) |

where is BH radius at extremality, determined by the solution of the cubic equation

(18) |

and is the length

(19) |

The BH thermodynamical parameters temperature , mass and entropy can be expressed in terms of the horizon radius as Cai:2003kt ()

(20) | ||||

(21) | ||||

(22) |

The spherical geometry of the horizon introduces another scale in the system, i.e. the radius of the sphere, which couples in a non-trivial way to the higher-curvature terms in the equations of motion (10). This scale introduces dependence on the GB coupling in the mass bound (16) and in the thermodynamical expression 22, 20 and 21. As a result, the thermodynamical and near-horizon behaviours of the GB BHs are completely different from their brane counterparts. Indeed, for charged GB black branes, such behaviours are universal, i.e. do not depend on , and are essentially the same of the RN black branes of GR Cadoni:2016hhd ().

Notice that although the extremal radius is determined only by the BH charge and the cosmological constant, the length and hence the extremal geometry (17) depend on the GB coupling constant. Notice also that the expression in the parenthesis in Eq. 20 is proportional to meaning that the extremal geometry is obtained at zero temperature.

### 3.2 Phase structure of AdS-Reissner-Nordström black holes

Although the metric function in Sect. 3 is singular for , the thermodynamical behaviour of the charged AdS-RN solution can be simply obtained by putting in Eqs. 22, 20, 21 and 16.

To characterise the phase structure of these BHs, a distinction between two cases can be made: fixed electric potential or fixed electric charge Chamblin:1999tk (); Chamblin:1999hg (). In this paper we only discuss the canonical ensemble, i.e. we work at fixed charge. We will not consider the grand canonical ensemble, i.e. the case of fixed chemical potential. As the charge of BH decreases to a critical value , the system undergoes a second-order phase transition. Below the critical charge, there are three possible branches of solutions that depend on the radius and therefore on the temperature of the system. For small temperatures, a small BH is the only locally stable solution; as the temperature increases, a meta-stable configuration describing intermediate BHs can be found; for sufficiently high temperatures, large BHs are globally preferred. The evolution from small to large BHs through the meta-stable region corresponds to a first-order phase transition. Above the critical charge, the BH solution is always globally preferred. This behaviour can be understood by analysing the temperature as a function of the BH radius given by Eq. 20 with . For it is a monotonic function, whereas it develops local extrema for and an inflection point for . Notice that the case is not included in the range of existence of the first order phase transition. In fact, corresponds to the AdS-Schwarzschild BH. The phase portrait of the AdS-RN BHs is very similar to a liquid/gas Van der Waals phase transition where the BH temperature plays the role of the pressure, the BH radius that of the volume and the BH charge that of the temperature Chamblin:1999tk (); Chamblin:1999hg (). This portrait has been extended by Kubizňák et al. in Refs. Kubiznak:2012wp (); Kubiznak:2016qmn () and to topological AdS BHs in massive gravity Hendi:2017fxp ().

We make a brief comment on the zero-charge limit. For , the metric (13) reduces to that of an AdS-Schwarzschild BH. However, from the thermodynamical point of view, this limit is singular. There is a discontinuity at , and the phase diagram of an AdS-Schwarzschild BH cannot be obtained as the limit of the AdS-RN one. In fact, the BH temperature as a function of the radius, Eq. 20, when becomes a monotonic function and shows no Van der Waals-like behaviour as in the RN case Cadoni:2017fnd ().

### 3.3 Phase structure of neutral Gauss-Bonnet black holes

Neutral GB BH solutions and their thermodynamical parameters are obtained by putting in Eqs. 22, 20, 21 and 3. These BHs are characterised by the absence of a regular, zero temperature extremal limit which, in turn, means the absence of an IR fixed point for the dual QFT in the holographic description. For positive , the extremal limit is a state with , zero entropy and positive non-vanishing mass. Therefore, the small temperature thermodynamical behaviour is always singular.

Neutral GB BHs exhibit an interesting phase structure. Different from Einstein
gravity, where small BHs are not stable and a thermal AdS state is energetically
preferred Hawking:1982dh (); Birmingham:1998nr (), in GB gravity there exists a
stable small BH.^{3}^{3}3Small BHs can be gravitationally unstable for values of
larger than those considered here Konoplya:2017ymp ().
It starts with a small positive free energy, becomes unstable
and evolves to a thermal AdS phase. Additionally, we also have the usual stable
BH phase for large radii Cho:2002hq ().
By inspecting the behaviour of the specific heat and the free energy, it is found
that the phase structure of neutral GB BHs strictly depends on the values of the
GB coupling constant and the BH radius Cai:2001dz (). For values of the GB
coupling constant below the critical one, , there are three different
branches of solutions that correspond to small, intermediate and large BHs.
The specific heat is positive in the first and third branch, whereas it is negative
in the second branch. This behaviour is a consequence of the fact that
given by Eq. 20 with is monotonically increasing for
, whereas it develops local extrema for Cai:2001dz ().
For the second branch disappears and BHs are always locally stable
but not necessarily globally preferred. Computing the free energy one finds that
the BH solution is globally stable and energetically preferred with respect to
thermal AdS in the parameter region , where
and are some functions of the horizon radius Cai:2001dz ().
Outside this region a Hawking-Page phase transition exists, BHs become globally
unstable and thermal AdS is energetically preferred.
Therefore, in the parameter region where BHs are energetically preferred with respect
to thermal AdS, the phase diagram of uncharged GB BHs has the same Van der Waals
form described in the previous section for AdS-RN BHs, with the GB parameter
playing the role of the BH charge .

Analogously to the limit, the limit is singular from the thermodynamical point of view. In fact for the phase diagram of an AdS-Schwarzschild BH cannot be recovered. First, the metric (3) becomes singular. Second, similarly to what we have seen for charged BHs in GR, the temperature as a function of the horizon radius exhibits a a discontinuous behaviour in the limit. The limits and have a similar singular behaviour also in the case of charged GB BHs.

### 3.4 Phase structure of charged Gauss-Bonnet black holes

The thermodynamical description of charged GB BHs is determined by the GB coupling
constant and the charge .
There are critical values of these parameters such that these BHs can exhibit
the typical Van der Waals gas behaviour in the - plane Hu:2013cia (); Zeng:2016aly ().^{4}^{4}4This is analogous to consider the cosmological constant as a pressure
term in the BH equation of state Frassino:2014pha ().
Thus, charged GB BHs possess both the Hawking-Page phase transition Hawking:1982dh (); Cvetic:2001bk ()
and a second-order one Zeng:2016aly ().
The former represents the transition from a stable AdS thermal state
to a stable BH spacetime.
When is the -dependent critical value of the temperature and .
Then, for and (or and )
AdS is preferred with respect to the BH, whereas for and (or and ),
the BH is preferred with respect to AdS.
It is remarkable that due to presence of and , the standard critical point
becomes a critical line in the - phase diagram Cvetic:2001bk ().

Again, the phase portrait has the Van der Waals-like form described in Sects. 3.2 and 3.3 if one considers only the parameter region where the BH phase is globally preferred with respect to the thermal AdS phase and if one holds either or fixed. In the former (latter) case, at the critical value () the system undergoes a second-order phase transition. For (), varying the temperature we have again a stable small BH phase and a stable large BH phase connected by a meta-stable phase. Moreover, the function always has the typical behaviour described in Sects. 3.3 and 3.2.

### 3.5 Linear perturbations in Einstein-Gauss-Bonnet gravity

In this section, we study linear tensorial perturbations about the background (12) in Einstein-Gauss-Bonnet gravity, i.e. . After suitable manipulations, the linearised equations of motion (10) are

(26) |

where and the explicit form of the tensors and can be found in Refs. Dotti:2004sh (); Dotti:2005sq (). In the transverse and traceless gauge (), with unless we can write

(27) |

where is the direction of the sphere along which the perturbation propagates and is the eigentensor of the Lichnerowicz operator built on the background -sphere

(28) |

The perturbations are both gauge-invariant and decouple Dotti:2004sh (); Dotti:2005sq (); Ishibashi:2003ap (); Kodama:2003jz (); Gibbons:2002pq (). This decoupling is a consequence of the spherical symmetry of the background and occurs for every value of and not only in the hydrodynamic limit . Furthermore, assuming a harmonic time-dependence of the perturbation, , the perturbation factorises leading to a set of equations which depend only on and Dotti:2004sh (); Dotti:2005sq (). Thus Eq. 26 reduces to a massive scalar equation

(29) |

where and the mass term is

(30) |

Notice that the mass term depends on the angular part of the perturbation through the eigenvalue of the Lichnerowicz operator (28) and on higher-curvature corrections through the GB constant . In the black brane case, if translational invariance is preserved, the mass term is identically zero Kovtun:2004de (). We stress that, although Eq. 29 holds for any , since we are interested in computing the shear viscosity (8), in the following will be taken equal to its minimum value implying .

There are no general exact analytical solutions of Eq. 29, but approximate analytical solutions can be found for and in the near-horizon limit. In the generic case, solutions can only be computed numerically.

The asymptotic solutions of Eq. 29 with are given in terms of the modified Bessel functions of first and second kind. For , the non-normalisable mode and the normalisable mode behave as

(31) | ||||

(32) |

In Eq. 31 the integration constant is chosen such that the non-normalisable mode goes to 1 as .

The near-horizon behaviour of is different for non-extremal and extremal BHs. In the case of non-extremal BHs at temperature and extremal BHs we write the metric function, respectively

(33) | ||||

(34) |

where the extremal BH radius is defined in Eq. 18 and the length is given by Eq. 19. In the non-extremal case, we write using a power-series expansion, and we solve Eq. 29 order by order. At leading order we find:

(35) |

For the extremal case, the leading quadratic behaviour of implies . The behaviour of in the near-horizon region is

(36) |

## 4 The shear viscosity to entropy density ratio

In this section, following the method proposed in Refs. Hartnoll:2016tri (); Lucas:2015vna (), we compute the shear viscosity to entropy ratio for the QFTs dual to the BH solutions discussed in Sect. 3. For Einstein gravity coupled to matter, of the dual QFT is determined by means of the retarded Green function in Eq. 8 and it is given by the non-normalisable mode of the perturbation evaluated at the horizon,

(37) |

This method can be generalised to include higher-curvature contributions. The computation uses a Wronskian method to determine the relation between the normalisable mode and the non-normalisable mode . Since this relation does not depend on the mass term in Eq. 29, the formula of Ref. Hartnoll:2016tri () also holds for BHs in GB gravity:

(38) |

where is the non-normalisable solution of Eq. 29 with .

For background solutions which do not break translational invariance, e.g. branes, the mass term is identically zero and the zero-frequency solution is everywhere Hartnoll:2016tri (); Cadoni:2016hhd (). On the contrary, in BH backgrounds, the translational invariance is broken, the mass term is non-vanishing, the solution for is not constant and must be calculated by integrating Eq. 29 with .

Large radius BHs , correspond to the large temperature regime . In this approximation can be inverted in Eq. 20 to get . Then, using Eqs. 31 and 38 we get

(39) |

As expected, in the large regime, does not depend on the charge. For GR BHs, Eq. 39 is a decreasing function of the temperature, thus the KSS bound is violated and the universal value is attained only for . For GB BHs, the behaviour is qualitatively similar but as the value of tends to .

In the extremal case, the metric function and its first derivative vanish when evaluated on the horizon and following Ref. Hartnoll:2016tri () the shear viscosity to entropy ratio is given by

(40) |

Equation 36 tells that , which substituted in Eq. 40 means that goes to zero in the extremal limit. The scaling at low temperatures of follows from simple matching argument Hartnoll:2016tri () between scaling of the Green function and the near-horizon scaling (36)

(41) |

where is given by (36). The scaling exponent satisfies for

(42) |

The global behaviour of as a function of is obtained by numerically integrating Eq. 29 supplied with a power-series boundary condition for . In the following, we choose units . For each value of the charge and the GB parameter, there exists a minimum mass (and hence a minimum radius) given by Eq. 16. Equation 29 is then integrated outwards from the horizon to infinity. Next, a shooting method is used to determine by requiring that . Finally, the temperature and for each solution are computed with Eqs. 38 and 20.

### 4.1 AdS-Reissner-Nordström black holes

The plots of resulting from our numerical calculations for GR are shown in Fig. 1 for electrically neutral (left panel) and charged (right panel) BHs.

The KSS bound is always violated for small and intermediate values of temperature, whereas it is saturated from below for large temperatures. In this section we extend the discussion of Ref. Cadoni:2017fnd (). For neutral AdS BHs, starts at the universal value at large temperatures and decreases monotonically as decreases, reaching a minimum non-zero value for the non-vanishing minimum temperature . Such a temperature corresponds to the minimum value of the BH radius, . At there is the Hawking-Page transition and for there are no stable BH solutions Birmingham:1998nr () and thermal AdS is energetically preferred with respect to the BH. The dotted line in the left panel of Fig. 1 gives for BHs with radii less than , whose behaviour is a consequence of the growing of for .

For AdS-RN BHs, decreases from at large temperatures (independently from the charge), but the behaviour for small and intermediate temperatures depends on the charge. As explained in Sect. 3.2, there exists a critical value of the charge under which the system undergoes a phase transition. On the right panel of Fig. 1, we plot our numerical results for for the critical charge and for representative values of the charge above, at and below the critical value. The dots (squares) in the curves with mark the critical temperature () corresponding, to the two local extrema of the function of Eq. 20. At these critical temperatures, the specific heat changes sign according to the discussion in Sect. 3.2. For it is found that and the function has an inflection point. For the function is monotonically increasing and BHs are always stable. The numerical values and are listed in Table 1 for a representative value of the charge below and at .

Interestingly, develops hysteresis for This is evident for the solid black curve in the right panel of Fig. 1. We have also checked that curves with have a similar hysteretic behaviour, whereas those with (as the orange dashed line) do not show this feature. Notice that the limit in the plot of l.h.s. of Fig. 1 is singular. As explained in Sect. 3.2, we have a discontinuity for , i.e. there is no phase transition at . Because the existence of the phase transition is a necessary condition for having hysteresis in , this means that also as a function of the temperature is discontinuous at : there is a more pronounced hysteretical behaviour for , but hysteresis disappears completely at . This hysteretic behaviour is a direct consequence of the Van der Waals-like behaviour of the AdS-RN BHs discussed in Sect. 3.2. It is related to the presence of two local extrema in the function in Eq. 20 or equivalently, to the presence of two stable states (small and large BHs) connected by a meta-stable region (intermediate BHs). This phase portrait has been considered as a general explanation of hysteretic behaviour for some variables of the system Knittel:1977 (). In particular, when the system evolves from high (low) to lower (higher) temperatures, a potential barrier prevents the evolution of the system from occurring as an equilibrium path between the two stable states Bertotti:1998 (). Equilibrium will be reached passing through a meta-stable region and a path-dependence of is generated. In particular, starting from high temperatures, the system will reach low temperatures going directly from the minimum and vice-versa. The presence of these local extrema determines the patterns of signs of the BH specific heat and free energy, hence the local thermodynamical stability Chamblin:1999tk (); Cai:2001dz (). Thus, hysteresis in and thermodynamical phase transition have the same origin and pattern. In fact, as already noted in Sect. 3.2, the phase diagram of AdS-RN BHs is very similar to that of a Van der Waals liquid/gas transition.

This is a very interesting result: for the dual QFT carries direct information about the thermodynamic phase transitions of the system. In the holographic context, a hysteretic behaviour in the shear viscosity has been already observed in Ref. Erdmenger:2010xm (); Erdmenger:2011tj () for AdS BHs with broken rotational symmetry and with a p-wave holographic superfluid dual. Moreover, it is well-known that nanofluids may exhibit hysteresis in the - plane Nguyen:2008 ().

### 4.2 Neutral Gauss-Bonnet black holes

Our numerical results for as a function of for neutral GB BHs are shown in Fig. 2 for selected values of the GB parameter in the range .

For large temperatures, the KSS bound is always violated due to the GB contribution and . At intermediate temperatures, the behaviour is qualitatively similar to that of RN BHs, with the GB parameter playing the role of the charge . As discussed in Sect. 3.3, there exists a critical value under which GB BHs can undergo a phase transition: by numerical investigation this value is , in good agreement with Refs. Zeng:2016aly (); Cai:2001dz (). Curves with (black solid and red dotted lines) show a hysteretic behaviour of as a function of the temperature, whereas those with do not. For a given value , there are two critical temperatures , which are marked respectively by dots and squares in the curves of Fig. 2. Their numerical values for selected values of are listed in Table 1. Notice that similarly to the case, the limit in the plots of Fig. 2 is singular. As explained in Sect. 3.3, for there is a discontinuity. This implies that also as a function of the temperature is discontinuous at . There is a more pronounced hysteretical behaviour for smaller and smaller values of , but hysteresis disappears completely at .

The physical interpretation of the appearance of hysteresis in for the QFT dual to the neutral GB BH is completely analogue to that discussed for the AdS-RN BH. When reaches the critical value, the system undergoes a second-order Van der Waals-like phase transition and exhibits the hysteretic behaviour in .

### 4.3 Charged Gauss-Bonnet black holes

The presence of both a non-vanishing charge and GB coupling constant makes the case of charged GB BHs more involved. However, as discussed in Sect. 3.4, the phase portrait becomes much simpler and has a Van der Waals-like form if we restrict our considerations to the region where BHs are globally stable and either holds or fixed. In this situation we expect the qualitative behaviour of as a function of to be quite similar to that found for the AdS-RN and the neutral GB BHs.

The numerical results for as a function of , confirm our expectation and are shown in Fig. 3 for fixed and selected values of the GB parameter (left panel) and for fixed and selected values of the charge (right panel). In both cases, the numerical results corroborate the analytical ones. For large temperatures, the KSS bound is always violated as . At intermediate temperatures, the behaviour of depends crucially on the values of the parameters and . For large values of (or for values of near to the unitarity bound ), large BHs are always stable, decreases monotonically with and there is no hysteresis.

Notice that the limits , respectively , are singular in the plot on the left, respectively on the right, of Fig. 3. Here we have a discontinuous behaviour of similar to that found in the limit for charged BHs in GR and to the for the uncharged BHs of GB gravity.

The situation changes drastically for (or ) of order and smaller: the system may undergo a Van der Waals-like phase transition. The function develops two local extrema and , signalising the presence of two different stable thermodynamical phase (small and large BHs) connected by a meta-stable one, correspondingly, the curve as a function of develops hysteresis. Two typical examples of this hysteretic behaviour are shown in Fig. 3. On the left panel, for fixed , the onset of hysteresis can be seen, corresponding to the thermodynamical phase transition, when . On the right panel, for fixed , we see the onset of hysteresis and the thermodynamical phase transition when . The corresponding values of the critical temperatures are marked by the dots () and squares () in Fig. 3 and their numerical values are listed in Table 1 for selected values of the parameters and . Analogous results can be found by choosing different and . Notice that, for stable BH solutions with values of and above the critical values, our numerical computation cannot reach , because it uses a power-series near-horizon expansion which does not hold in the extremal case. However, from Eqs. 36 and 41, which describe analytically the near-extremal behaviour we conclude that smoothly as .

1/100 | 0 | 1/100 | 1/100 | 2/100 | |||||||
---|---|---|---|---|---|---|---|---|---|---|---|

0 | 1/1000 | 1/100 | 1/1000 | 5/1000 | 1/100 | ||||||

0.449 | 0.441 | 0.448 | 0.431 | 0.390 | 0.448 | 0.440 | 0.397 | 0.431 | 0.429 | 0.425 | |

0.664 | 0.441 | 1.787 | 0.587 | 0.390 | 0.638 | 0.559 | 0.397 | 0.494 | 0.445 | 0.425 |

## 5 Summary and outlook

In this paper we have used the AdS/CFT correspondence to obtain information about the behaviour of bulk BHs by studying the hydrodynamic properties of the dual QFTs. In particular, we have defined and computed the shear viscosity to entropy ratio in the transverse channel for QFTs holographically dual to five-dimensional AdS BH solutions of GR and GB gravity. In this way, we have extended the usual derivation of for QFTs dual to gravitational bulk backgrounds with planar horizons to backgrounds with spherical horizons. We have shown that in holographic models the shear viscosity to entropy ratio of the QFT is closely related and keeps detailed information about the thermodynamical phase structure of the dual BH background. This is not completely unexpected, because experience with another holographic condensed matter system, like holographic superconductors, has shown us that transport features of the dual QFT may be strongly related to phase transitions of the dual black brane.

In general, the definition of a transport coefficient such as the shear viscosity is associated with the translational invariance of the system, i.e. the conservation of the momentum. As a consequence the Fick law of diffusion can be derived from the associated conserved current. For systems that break translational invariance, the hydrodynamic interpretation in terms of conserved quantities fails but hydrodynamics can be still defined as an expansion in the derivatives of the hydrodynamic fields. In this way, it is possible to define the shear viscosity through a Kubo formula also for QFTs on a spherical background, see Eq. 8, where the stress-energy tensor is only covariantly conserved. In addition, one can understand as the rate of entropy production due to a strain, which is the typical interpretation when the homogeneity is broken by external matter fields. From this point of view, QFTs dual to spherical BHs are very similar to QFTs dual to black branes where the translational symmetry is broken by non-homogeneous external fields, e.g. scalars Hartnoll:2016tri (); Burikham:2016roo (); Alberte:2016xja ().

The definition of the hydrodynamic limit of a QFT on the sphere is plagued by an issue related to the compactness of the space. In fact, in a compact space, the usual hydrodynamic limit as an effective theory describing the long-wavelength modes of the QFT has not a straightforward interpretation. Our proposal is that for QFTs dual to bulk spherical BHs, the hydrodynamical, long wavelength modes can be described by the modes that probe large angles on the sphere. This is in analogy with the modes for QFTs dual to bulk black branes which probe large scales on the plane.

There is still a crucial difference between the two cases. When the breaking of translational symmetry is generated by external fields, the symmetry may be restored or not when the system flows to the IR Hartnoll:2016tri (). Instead, in the BH case, because the breaking has a geometric and topological origin, translational symmetry cannot be restored in the IR.

As expected, the large behaviour of , corresponding to the flow to the UV fixed point, reproduces the universal value or in the GB case. When the bulk BH solution has a regular and stable extremal limit (like e.g. charged BHs) and remains stable at small , as with a scaling law. In the latter case, the system flows in the IR to the geometry.

Our most important result is the behaviour of at intermediate temperatures. A second-order, Van der Waals-like, phase transition occurs when the control parameters go below their critical values Chamblin:1999tk (); Chamblin:1999hg (). In this situation BHs may also undergo a first order phase transition controlled by the temperature. This corresponds to the transition from small to large BHs connected through a meta-stable intermediate region. As a consequence, as a function of always develops hysteresis and it becomes multi-valued as expected for a first order phase transition Erdmenger:2010xm (). Notice that in this case the first and second-order phase transitions are both necessary in order to have the hysteretic behaviour in . Even though, similarly to the case discussed in Ref. Erdmenger:2010xm () the multi-valuedness of is directly related only to the first order one. The role of the second-order phase transition is to allow for the existence of the first order one.

The mechanism that generates hysteresis in is the same that is responsible for the phase transition and can be traced back to non-equilibrium thermodynamics. When a control parameter, i.e. the charge or the GB coupling constant , is below its critical value, the function develops both a local maximum and minimum. The regions below the maximum and above the minimum correspond to two stable solutions, i.e. small and large BHs, respectively. The region between these two is represented by an unstable (meta-stable) region of intermediate BHs. When the system evolves from large (small) BHs to small (large) BHs, a potential barrier prevents the evolution of the system from occurring as an equilibrium path between the two stable states Bertotti:1998 (). Equilibrium will be reached passing through a meta-stable region Knittel:1977 (), and a path-dependence of is generated. The presence of these local extrema determines the patterns of signs of the BH specific heat and free energy, hence the local thermodynamical stability Chamblin:1999tk (); Cai:2001dz (). This interesting result represents the first attempt to infer about BH thermodynamics through a detailed analysis of a transport coefficient as the shear viscosity.

Our definition of for spherical backgrounds is channel-dependent. In general we have three different determinations of for shear, sound and transverse (scalar) perturbations. In this paper we have focused on transverse perturbations. It would be of interest to check whether the behaviour of the viscosity found in this paper for the transverse channel also extends to the sound and shear channels. The computation of our analogue in these other two channels is rather involved and we have left it for future investigations.

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