Fluid-gravity correspondence in the scalar-tensor theory of gravity: (in)equivalence of Einstein and Jordan frames

The duality of gravitational dynamics (projected on a null hypersurface) and of fluid dynamics is investigated for the scalar tensor (ST) theory of gravity. The description of ST gravity, in both Einstein and Jordan frames, is analyzed from fluid-gravity viewpoint. In the Einstein frame the dynamical equation for the metric leads to the Damour-Navier-Stokes (DNS) equation with an external forcing term, coming from the scalar field in ST gravity. In the Jordan frame the situation is more subtle. We observe that finding the DNS equation in this frame can lead to two pictures. In one picture, the usual DNS equation is modified by a Coriolis-like force term, which originates completely from the presence of a non-minimally coupled scalar field on the gravity side. Moreover, the identified fluid variables are no longer conformally equivalent with those in the Einstein frame. However, this picture is consistent with the saturation of Kovtun-Son-Starinets (KSS) bound. In the other picture, we find the standard DNS equation (i.e. without the Coriolis-like force), with the fluid variables conformally equivalent with those in Einstein frame. But, this second picture, is not consistent with KSS bound. We conclude by rewriting the Raychaudhuri equation and the tidal force equation in terms of the relevant parameters to demonstrate how the expansion scalar and the shear-tensor evolve in the spacetime. Although, the area law of entropy is broken in ST gravity, we show that the rewritten form of Raychaudhuri's equation correctly results in the generalized second law of black hole thermodynamics.


I. INTRODUCTION
Despite the enormous success of Einstein's theory of general relativity (GR), there are several indications [1][2][3][4][5][6][7][8][9] implying that Einstein's GR might not be a complete theory of gravity. There are several motivations, emerging from both theory [10][11][12][13] and from experiment [1,4,5], that motivate the study of alternative theories of gravity. In the literature, one can find several mature alternative theories of gravity with various motivations to study each of these theories (see the review [14]). The scalar-tensor theory of gravity is one of the most popular among various alternative theories of gravity. ST theory not only combines two types of fields together which mediate gravity, but also the theory is built on the strong foundation of Einstein's GR. As a result, this theory has been the subject of intense research in recent times [15][16][17][18][19][20]. Recently, we have resolved the longstanding issue related to the thermodynamic description of scalar-tensor gravity. We have obtained the thermodynamic laws in the Jordan and Einstein frames by properly defining the thermodynamic parameters. This showed the equivalence of these thermodynamic parameters in the two frames [21,22].
Apart from the connection of GR with thermodynamics, there is another intriguing connection which implies that gravity could be an emergent phenomenon rather * krishnakanta@iitg.ernet.in † bibhas.majhi@iitg.ernet.in ‡ dougs@mail.fresnostate.edu than a fundamental force. This connection was obtained first by Damour who showed that Einstein's equation, when projected onto a null hypersurface, has the structure of the Navier-Stokes (NS) equation of fluid dynamics [23]. This projection of Einstein's equation is known as the Damour-Navier-Stokes (DNS) equation. The DNS equation contains an extra non-linear term that does not have any fluid-dynamic interpretation. This makes the DNS equation distinct from the usual NS equation. Later, this fluid dynamic connection was again established by Price and Throne using the membrane paradigm [24]. They referred to the equation they obtained as the Hajicek equation instead of the NS equation due to the presence of the extra non-linear term. This extra non-linear term can be removed if one replaces the convective derivative by Lie-derivative [25], or by choosing the local inertial frame as the observer's frame [26,27]. After this, several works investigated various aspects of this fluid-gravity connection . Most of the work mentioned above on the fluid-gravity connection are based on Einstein's GR. A question naturally arises: "is the fluid-gravity analogy a characteristic of Einstein's gravity only, or can a similar connection be found in other alternative gravity theories?". It is also interesting to examine how the expressions of fluid parameters (such as pressure, momentum, external force etc.) and coefficients (such as the bulk viscosity coefficient, shear viscosity coefficient etc.) get modified in these alternative gravity theory (e.g. scalar-tensor theory or the higher curvature theory). Moreover, in scalartensor theory, there has always been a major debate concerning the two conformally related frames in which the theory is described (the Jordan frame and the Einstein frame). The debate is whether this mathematical conformal equivalence results in the physical equivalence of the two frames (see the review [50]). Regarding this, the recent opinion is that the Jordan and Einstein frames are physically equivalent in the classical limit. However, these two frames might not be physically equivalent in the quantum regime [51,52]. Thus, if the DNS equation can be established in the two frames and the fluid parameters and the coefficients can be identified, it will be interesting to check whether the parameters and the coefficients are equivalent in the two frames or not.
To answer these questions, in this paper we investigate the fluid-gravity correspondence in scalar-tensor gravity. Since, in the Jordan frame, the scalar field φ is nonminimally coupled with the Ricci-scalar R, we show that the usual way of obtaining the DNS equation does not work in the Jordan frame (we discuss this in more detail in our analysis below). Instead, one can obtain the gravitational fluid dynamic equation in the Jordan frame via two different routes. In one method, we obtain the gravitational DNS equation with the Coriolis-like force term. In this case, the fluid variables are not equivalent to those of the Einstein frame. However, this method is favored by some recent works (such as [53]) as, in this case, the shear viscosity coefficient η is obtained as η = φ/16πG. As a result, the ratio of η to entropy density (s) saturates the Kovtun-Son-Starinets (KSS) bound [54]. We call this picture "case 1". However, we show that there is another possible way to obtain the DNS equation, where, the fluid variables are conformally equivalent. We call this picture, "case 2". This latter method of obtaining the DNS equation agrees with the thermodynamic viewpoint. In the Einstein frame, we show, that obtaining the DNS equation is similar to the usual GR case. However, one difference is that one can obtain the external force term in the DNS equation in the Einstein frame (also in the Jordan frame) even in the absence of external matter fields, unlike the case in standard GR. After obtaining the DNS equation in the two frames, we investigate the evolution of the expansion scalar (which is given by the Raychaudhuri equation) and the shear tensor (which is given by the tidal force equation). We rewrite the Raychaudhuri equation and the tidal force equation in terms of the expansion scalar and the shear tensor. We show that the Raychaudhuri equation in the Jordan frame, when it is written in terms of the parameters defined for the equivalent fluid-dynamic description (case 2), results in the generalized second law of black hole thermodynamics.
The paper is organized as follows: In the following section, we provide a brief review of the scalar-tensor theory of gravity. Thereafter, in the next section, we first describe the null-geometry and then obtain the DNS equation in the Jordan and Einstein frames. In the following section, we describe the evolution of the expansion scalar in the two frames by obtaining the Raychaudhuri equation in terms of the variables obtained earlier. There, we also prove the entropy increase theorem which follows from the obtained Raychaudhuri equation and from the null-energy condition. Then, in the penultimate section, we obtain the tidal force equation in each frame and show the evolution of the shear tensor. We end our work with the conclusions of our analysis.

II. BRIEF REVIEW: EQUATIONS OF MOTION IN THE TWO FRAMES
Here, we briefly review the elements of ST gravity which we will use in this work. We begin by providing the relevant transformation relations between the Jordan and Einstein frames, and we introduce the corresponding field equations of motion. These will be our main requirements since the fluid description of gravity comes from the projection of gravitational equation on to a null hypersurface. A more detailed analysis of scalar-tensor theory, at the level of the action, can be found in [21,22]. For more about this action description and other important issues, one can look at our previous works [21,22].
Usually, scalar-tensor theory is described in two frames. In the original frame, known as the Jordan frame, the action is given by In this frame, the scalar field φ is non-minimally coupled to the Ricci-scalar R. Moreover ω(φ), the Brans-Dicke parameter, is considered as a general function of φ. When ω(φ) is taken as a constant, the theory reduces to Brans-Dicke theory [55]. Here, V (φ) in (1) is an arbitrary scalar field potential. The equations of motion for g ab and φ are obtained by varying the action (1) yielding and Rg ab is the Einstein tensor. The non-minimal coupling in (1) can be removed by a set of transformations: (i) a conformal transformation of the metric of the form g ab →g ab = Ω 2 g ab , and (ii) a scaling of the scalar field given by From now on the untilde variables correspond to the Jordan frame while the tilde variable correspond to the Einstein frame. Using the above relations (4) and (5), the non-minimal coupling in (1) can be removed and one can go from the Jordan frame to the conformal (i.e. Einstein frame). The action in the Einstein frame is where U (φ) = V (φ)/(16πGφ 2 ). The equations of motion ofg ab andφ can be obtained from the variation of the action (6), which yields One can check that under the transformations (4) and (5) the above equations reduces to Eqs. (2) and (3). So both frames are equivalent, at the equations of motion level. We end this section by mentioning one key aspect not often highlighted in the literature. Although, the action in the two frames ((1) and (6)) are connected by the set of transformations (4) and (5), one can note that the actions in the two frames are equivalent only up to a total derivative term, which is the given as follows (for details see [21,22]): Since the two actions are connected by a total derivative term, it can be neglected if one is interested in the equations of motion i.e. the dynamics of the system. In our previous work [21,22], we have shown that in constructing the thermodynamical quantities, like entropy, energy etc., the extra total derivative term does play a crucial role. This is because these boundary terms in the action do contribute to the thermodynamic parameters, since they are defined on the relevant boundary of the full manifold. We observed that the total derivative term indeed helps in resolving several inequivalences (such as thermodynamic entities and the holographic relations between the surface and bulk terms of the action) between the two frames. Of course, in the present case, the DNS equation and the dynamics of the null surface are obtained from the equations of motion of the metric tensor. Therefore, the extra φ term in (9) has no significance in the present case.
In the following section we will obtain the DNS equation for ST theory. In Einstein's gravity, when Einstein's equation is projected on to a null surface, it has a structure, similar to the Navier-Stokes equation of hydrodynamics [23]. In the present scenario with ST theory, we follow a similar approach. However, in this case, there are several extra terms in the equation of motion in the two frames. Also the scalar field φ is non-minimally coupled with the Ricci-scalar in the Jordan frame. Therefore, it will be interesting to investigate whether the DNS equation can be obtained in the present case of ST theory. If so, then we have to check how the expressions of the fluid parameters get modified. Also, we will examine whether the fluid parameters are conformally invariant between the two frames.

III. DNS EQUATION IN JORDAN AND EINSTEIN FRAMES
As mentioned above, the structure of the Navier-Stokes-like equation for GR was obtained first by Damour [23]. Later a more detailed investigation was performed by Price and Throne [24]. After these early works various researchers expanded on this idea . However, the approach which we follow here, depends largely on the structure of the null-hypersurface and the spacetime foliation of the null surface. Therefore, in the following we give a brief discussion of the null-hypersurface and its (1 + 3) foliation. More discussion in this regard, can be found in [25].
A. Spacetime foliation on null hypersurface Let (M, g ab ) be the whole (1 + 3)-dimensional manifold, where lower case Latin indices run {0, 1, 2, 3}. A null hypersurface (H , γ αβ ) is a three dimensional hypersurface embedded in a four-dimensional manifold M such that it satisfies the condition γ αβ v β = 0, where v α is the vector defined in the tangent space of H . Another way of saying this is that the pullback of the induced metric of a null-hypersurface onto its tangent plane is degenerate. Here, the Greek indices denote the coordinates associated to the null surface H (defined by x 3 =const.) and run {0, 1, 2} . Moreover, null hypersurfaces are characterized by the null vectors l a , which is orthogonal to H and satisfies the geodesic condition of the spacetime. Since the normal of the null surface H is self orthogonal, i.e. l a l a = 0, one major difference of the null hypersurface H with the spacelike or timelike one is that one cannot define an orthogonal projection operator onto H . To study the dynamics of a null hypersurface extrinsically we also adopt the standard (1 + 3) foliation of the spacetime as described in [25].
In the present case, each spacelike hypersurface (which we denote as Σ t , characterized by the unit timelike normal n = N dt with N being the lapse function) will inter-sect the null hypersurface H on a two-dimensional surface S t i.e. S t = H Σ t . Therefore, S t will be characterized by two normals: one is the timelike normal n and the other is a unit spacelike normal, denoted by s. These satisfy the properties s · s = 1, n · n = −1 and n · s = 0 . Therefore, one can define an induced metric on the two surface S t , which is orthogonal to both n and s . The induced metric on S t is defined as Moreover, the two-surface S t can also be regarded as the intersection of two null-hypersurfaces: one null surface H, of course, is characterized by the outgoing null vector l = N (n + s) and the other one is characterized by the auxiliary (or ingoing) null vector k = (1/2N )(n − s), with the conditions l · l = k · k = 0 and l · k = −1 . The induced metric on the two surface S t , defined in (10), can now be written in terms of the null vectors l and k as We shall use this form of the induced metric from now on. Note that q ab l a = q ab k a = 0, and q b a q c b = q c a . Therefore, the induced metric q ab is orthogonal to the null vectors l and k, and the mixed tensor q a b allows one to project everything onto the two surface S t .
This discussion and results are independent of what frame we are using, and are equally valid in both Einstein and Jordan frames. For example, the induced metric in the Einstein frame is identical to the form in (10) and (11) but with the quantities are denoted by the tilde variables: q ab =g ab +ñ añb −s asb =g ab +l akb +l bka .
Having all the necessary details, we are now ready to find the DNS-like equation by projecting the field equations. We begin the with the Einstein frame variables.

B. DNS equation in the Einstein frame
The procedure for obtaining the DNS equation in the Einstein frame is straightforward since the equation of motion in the Einstein frame (i.e. Eq. (7)) is similar to the equation of motion from standard GR.
The analysis starts by defining various important quantities on the null surface, which will ultimately be connected with the fluid variables. We defineθ ab as which is the pullback of the covariant derivative of the null vectorl onto S t . In the above relation (13), we have definedω The expression ofθ ab in (13) does not imply thatθ ab is symmetric. However, if one replaces the terml ak i∇ ilb in (13) using the Frobenius theorem, i.e.l [a∇ilb] = 0, one can straightforwardly obtain thatθ ab is a symmetric tensor in a and b .θ ab can be decomposed into two parts: one being the symmetric trace-less partσ ab and the other is the trace partθ given bỹ The trace partθ is given bỹ In the above,κ is the non-affinity of the null geodesics and is defined by the relatioñ Note that when a null-surface corresponds to a black hole horizon,κ can be identified as the surface gravity of the black hole horizon.
Having the definition of different quantities on the null hypersurface, let us now project the equation (7) on to this surface. Note that one part of this equation contains Einstein's tensor. The relevant part of this can be projected in the following way: from ) and using (13) and (16) we obtaiñ Using (13), one can further re-write the last term on the RHS of (18) as Substituting (19) in (18) we obtaiñ Equation ( whereΩ a =q b aω b =ω a +κk a . In the above we used l aω a =κ andk aω a = 0. Also we denoteD a (θ +κ) = q b a∇b (θ +κ) whereD a is the covariant derivative with respect the hypersurface's metric (i.e.q ab ). From equation (7) and using the identity (21) where, This can be identified as the energy-momentum tensor of the scalar-fieldφ . The first two terms on the right hand side (RHS) of (22) can be replaced. First from the definitioñ and usingθ j alj =θ j akj = 0, we obtaiñ Therefore, we get Substituting (26) and (27) in to (22) one obtains where, we have usedθ m n =σ m n + 1 2q m nθ . The RHS of equation (28) are the DNS terms in standard GR [25,26]. In this case our left hand side (LHS) is non-zero. Therefore (28) is our DNS-like equation in the Einstein frame for ST gravity. It should be pointed out that, if the Liederivative in (28) is expressed in terms of the convective derivative, one extra term,θ i aΩi , appears compared to the usual Navier-Stokes (NS) equation. This term does not have any fluid dynamic interpretation. This difference was highlighted in earlier works [24][25][26].
The corresponding fluid parameters of the DNS equation in the Einstein frame as given in (28) are identified as follows: the term on LHS,F a =T (φ) abl b , can be identified as the external force term; the momentum density is given asπ a = −Ω a /8πG; the pressure is identified as P =κ/8πG; the shear viscosity coefficient is given asη = 1/16πG; the bulk viscosity coefficient is given as ξ = −1/16πG (note that for the standard NS equation, the total viscous tensor is 2ησ a b + ξδ a b θ) . In the present case, one does not necessarily require any external matter source to have anF a term in the DNS equation (28). This is the major difference with standard GR. If one includes some external matter, one can still obtain the DNS equation. However in this case the energy-momentum tensorT is the energymomentum tensor coming from the additional external matter source. The external force in the DNS equation is then identified asF a =T abl b . We make one final comment before moving on to the Jordan frame. The entropy of scalar-tensor theory in the Einstein frame is identified as [21,22,56]S =Ã/4G, whereÃ is the surface area of the null horizon. This gives an entropy density ofs =S/Ã = 1/4G . As a result, the ratio of shear viscosity to entropy density is This is the same as in standard GR and is consistent with the Kovtun-Son-Starinets (KSS) bound [54].

C. DNS equation in Jordan frame
In obtaining the DNS equation in the Jordan frame, there are several points one has to recognize. First, the scalar field in the Jordan frame is non-minimally coupled with the Ricci scalar and the gravitational interaction is mediated both by the metric tensor as well as by the scalar field. Therefore, it is expected that the scalar field will invariably appear in the expressions of the fluid parameters and the transport coefficients. Moreover, we mentioned earlier that both the equations of motion for the metric (i.e. (2) and (7)) in the two frames are equivalent. Thus, a proper DNS equation in the Jordan frame will be one where the scalar field will appear in the expressions of the fluid parameters as well as having the equation be conformally connected to (28). Note that the DNS equation and the fluid parameters in the Einstein frame have been unambiguously obtained at the end of the last subsection. However, in the Jordan frame, the presence of φ gives rise to two different pictures/cases in the fluid description. In the first picture (i.e. case 1), the fluid variables are not conformally equivalent in the two frames. Further, in case 1, the fluid dynamic equation appears as the DNS equation along with an extra Coriolis-like force term. We mention, in connection with earlier works on the KSS bound, how this first picture is more favored. In the second picture (case 2) one finds that the fluid variables in the two frames are conformally equivalent, but now these variables violate the KSS bound. In the subsections below we first discuss the inequivalent picture (case 1), and then we move on to discuss the equivalent picture (case 2). We follow a procedure similar to that used above in the Einstein frame, to obtain various useful results, that help us to obtain the final form of the DNS equation in the Jordan frame. First we find θ ab as with ω a = l i ∇ i k a . As before, in the Einstein frame case, θ ab can be written as sum of a traceless part and a trace part: where, θ is given as In addition, we find Projecting the above expression onto the null surface, we obtain where Ω a = q b a ω b = ω a + κk a with l a ω a = κ; k a ω a = 0 and D a (θ + κ) = q b a ∇ b (θ + κ) . As in the Einstein frame, we can obtain two additional identities and q n a l i ∇ i ω n = q n a £ l Ω n − θ m a Ω m − κΩ a .
Substituting (35) and (36) in (34) one obtains R mn l m q n a = q n a £ l Ω n + θΩ a − D a ( The LHS of (37) can be written as R mn l m q n a = 8πGT mn l m q n a where, using the equation of motion (2), one can identify T mn as Therefore, one obtains 8πGT mn l m q n a = q n a £ l Ω n + θΩ a − D a ( Although equation (39) looks like the gravitational Navier-Stokes equation for the Jordan frame there are issues with making this identification. First, in the above relation (39), the scalar field φ does not appear in the expressions of the fluid parameters and the transport coefficients. The role of the scalar field in (39) appears like an external field, which is not consistent with the non-minimal coupling in ST theory in the Jordan frame. Second, if (39) is considered the DNS equation in the Jordan frame, then the shear viscosity coefficient is identified as η = 1/16πG. The entropy in the Jordan frame is [21,22,56,57] S = φA/4G, which gives the entropy density as s = φ/4G . So, the ratio of shear viscosity to entropy density will be obtained as η/s = 1/4πφ, which is not consistent with the KSS bound [54]. Because of these issues, we conclude that Eq. (39) is not the correct form of the DNS equation in the Jordan frame.
To address these issues we can incorporate φ in the expressions of the fluid parameters and the transport coefficients, to obtain a proper DNS equation in the Jordan frame. We begin by multiplying (37) by φ, and using some identities to move φ past some of the derivative operators.
Using the equation of motion (2), equation (40) can be written as where T (φ) mn = φT mn . The RHS of the above equation, other than the last term, has the structure of the DNS equation. The last term, 2l m q n a ω [m ∇ n] φ , can be identified as the rotational contribution in the full manifold. This term can be thought of as the rotational contribution in the DNS equation and therefore we identify it as a Coriolis-like force term. The expression of the DNS equation in (41) is the counterpart of (28) in the Einstein frame, as can be checked by applying the transformations (4) and (5).
We identify the fluid parameters and the transport coefficient in the following way: the external force is identified as F a = T (φ) ab l b ; the momentum density is identified as π a = −φΩ a /8πG; the pressure is given as P = φκ/8πG; the shear viscosity coefficient is identified as η = φ/16πG; the bulk viscosity coefficient as ξ = −φ/16πG. Thus, equation (41) can be interpreted as the hydrodynamic equation of a fluid in a rotating frame with the angular velocity W a = ∇ a φ/2.
Even without an external matter field, we get an external force term coming from the T (φ) ab term. When an external matter term is added the external force term is given by the combination of the energy-momentum tensor for φ plus the energy-momentum tensor of the external field i.e. T ab = T (φ) ab + T ext ab . As in previous cases the external force will be identified as F a = T ab l b . Note that, in this case, the ratio of the shear viscosity η (which here is equal to φ/16πG) to the entropy density is η/s = 1/4π. This value is consistent with KSS bound [54]. A similar η/s ratio has also been predicted in [53] for f (R) gravity, which can be considered as a subclass of scalar-tensor gravity. Therefore, the inequivalent picture, which has been described here, is more favored by the literature. Note that the scalar field φ, which is nonminimally coupled in this frame, appears in several fluid parameters (like π a , P , η, ξ). One way of interpreting the non-minimal coupling of φ with R is that in the Jordan frame, Newton's constant of GR is replaced by an effective Newton's constant as G −→ G ef f = G/φ [58]. With this viewpoint, the modification of the expressions of fluid parameters and the transport coefficients can be justified and those expressions can be seen as being the same as in GR except with G rescaled as G/φ.
Although the above case is consistent with earlier theoretical results in the literature, it shows that the fluid variables in the two frames are not equivalent (e.g. P = P ,π a = π a ,F a = F a etc.). We now clarify this inequivalence of the fluid variables. From the conformal transformation relation (4) and from the normalization conditions of n andñ (i.e. n · n =ñ ·ñ = −1) it follows thatñ a = √ φn a andñ a = (1/ √ φ)n a . Similarly from the normalization condition of s ands one finds s a = √ φs a ands a = (1/ √ φ)s a . Moreover, in the (1 + 3) foliation of the spacetime, the lapse function N is given as N = √ −g 00 so we findÑ = √ φN . Earlier we defined l and k as linear combinations of n and s, which yields l a = l a ,l a = φl ã The transformation relation of various quantities, that define the fluid variables in the Jordan frame and the Einstein frame, are given bỹ , From the relations in (43), one can conclude that the fluid variables in the two frames are not equivalent for the present case. As mentioned earlier, whether the two conformally connected frames are physically equivalent or not, has been an unsolved puzzle for several decades.
However, from the thermodynamic perspective, we have shown that the two frames are thermodynamically equivalent and the thermodynamic parameters are exactly equivalent between the two frames [21,22] (under certain assumptions, similar results have also been obtained in [56]). All of this leads to the question "Is it possible to obtain a DNS-like equation in the Jordan frame, where the fluid variables are equivalent across the two frames?".
In the next subsection we show that one can answer this question in the affirmative.

Equivalent picture -case 2
We now want to alter our previous analysis of the Jordan frame to find a DNS equation whose fluid variables are the same as those in the Einstein frame (i.e.κ,θ, σ a b ,Ω a etc.). We start by examining the expression: q n a ∇ mθ m n + (θ +κ)Ω a + q n a l m ∇ mωn − q n a ∇ n (θ +κ) − θ m a k i ∇ i l m . In this expression the fluid variables are taken intentionally as that of the Einstein frame (e.g. ω a ,κ,θ,θ ab ,Ω a etc.), but the background and the covariant derivatives are defined with respect to the metric of the Jordan frame. Using (43), we obtain To obtain this result, we have used (34). Now, one can straightforwardly obtain the following relation (45) From this expression and using (43), one further finds Also we have, q n a l m ∇ mωn = q n a l m ∇ m (Ω n −κk n ) = q n a £ lΩn −θ m aΩm −Ω aκ . Again, using the transformation relation (43), we arrive at We now substitute (46) and (47) into (44) which yields Equation (48) can be further simplified. From (30), one obtains q n a (∇ n l i )(∇ i ln φ) = Ω a l i ∇ i ln φ + θ i a (∇ i ln φ) . Using this with θ i a = σ i a + q i a 2 θ in (48), yields Equation (49) can also be identified as a DNS-like equation in the Jordan frame. From the equation of motion (2), we obtain Also, using the transformation relations in (23) one can obtain an expression forT ab in the Jordan frame as Comparing equations (50) and (51), one can conclude that in (49) the RHS, as a whole, contributes to 8πGT (φ) mn l m q n a . Thus the expression of the DNS-like equation (49) in the Jordan frame, is given as One can again identify (52) as the DNS equation in the Jordan frame, where the fluid variables are equivalent to those in the Einstein frame and are identified as follows: the external force is identified as F a =Tφ ab l b ; the momentum density is identified as π a = −Ω a /8πG; the pressure is given as P =κ/8πG; shear tensor is Σ a b ; the shear viscosity coefficient is identified as η = 1/(16πGφ); the bulk viscosity coefficient is ξ = −1/16πG . For this case the DNS equation in the Jordan frame, equation (52), all the fluid parameters are equivalent to those in the Einstein frame (i.e.F a = F a ,π a = π a ... etc.) except for the shear viscosity coefficient, which is connected as η =η/φ. Also the shear tensor in the Jordan frame for this case is connected to the the shear tensor in the Einstein frame as Σ a b = φσ a b and Σ ab =σ ab . We now examine what happens when an external matter field is included in the gravitational action. In the Jordan frame, the action of the external matter field is A ext = √ −gL ext d 4 x, whereas in the Einstein frame, it is given asÃ ext = √ −gL ext d 4 x . Since these actions for the external fields in the two frames are conformally invariant (i.e.Ã ext = A ext ), this implies that √ −gL ext = √ −gL ext andL ext = L ext /φ 2 . Now, in the Jordan frame, the energy momentum tensor corresponding to the external matter source is which is connected to the energy-momentum tensor in the Einstein frame as Introducing an external matter field results in the zero on the RHS of (2) being replaced by T (ext) ab /2. However, in (50), one gets the extra term 8πGT (ext) ab /φ . Thus, taking the external matter field into account, gives the following result for the external force in the Jordan frame: F a = (Tφ ab +(T In summary the introduction of an external matter field leads to a force that is invariant between the Jordon and Einstein frames, while the energy-momentum tensors are related by a factor of 1/φ as seen in (54).
We conclude this section by making a final important comment. The fluid-gravity connection is not wellexplored in the context of the scalar-tensor gravity. However, there are a few works for f (R) gravity [35,53], which suggest that the shear viscosity coefficient is η = f ′ (R)/16πG which lead to the following ratio with the entropy density η/s = 1/4π. This ratio saturates the KSS bound. Since f (R) gravity can be analyzed as a particular form of scalar-tensor gravity with the scalar field identified as φ ≡ f ′ (R), those works on f (R) gravity favor the inequivalent picture (case 1) of the Jordan frame described in the last subsection. But in the present picture (case 2) we have which is not a constant and depends on φ. Thus this ratio from (55) can violate the KSS bound depending on the value of φ. Nevertheless, in the context of the fluidgravity correspondence, an equivalent picture can also be drawn, as we have shown here.

IV. THE ENTROPY INCREASE THEOREM
Within the framework of standard GR, when R mn l n is projected onto the null surface by contraction with the projection tensor, q m a , it yields the DNS equation. On the other hand, when R mn l n is contracted with another null vector, l m , it results in the Raychaudhuri equation.
In an earlier section, we showed that the procedure of obtaining the DNS equation in scalar-tensor theory (in Jordan frame) is different from standard GR due to the scalar field φ. In this section, we discuss the Raychaudhuri equation in the context of the scalar-tensor gravity. Moreover, it is well-known that in standard GR, the generalized second law (GSL) of black hole thermodynamics can be proven from the Raychaudhuri equation. Since the area law of entropy breaks down in scalar-tensor gravity, in the Jordan frame, it is worth investigating whether the Raychaudhuri equation can prove the generalized second law of thermodynamics for scalar-tensor gravity.

A. Einstein frame
Obtaining the null Raychaudhuri equation in the Einstein frame in ST theory is straightforward (the same as in standard GR). Contracting (20) with a second null vector, l a , and using (13) one simply obtains l a∇ aθ =κθ −θ abθ ab −R abl alb .
Expressingθ ab in terms of the shear tensorσ ab and the expansion scalarθ, as given by (15), leads to equation (56) becoming Next, using the equation of motion in the Einstein frame, one obtains To obtain the above equation we have usedl a∇ aθ = dθ/dλ, whereλ parameterizes the null geodesics, as defined by the normall a = dx a /dλ . Also note that in the above equationT ab is given asT ab =Tφ ab +T ext ab . Now, we note thatTφ abl alb = (l a ∂ aφ ) 2 ≥ 0. Therefore, if the energy-momentum tensor of the external field satisfies the null energy condition in the Einstein frame (i.e.T ext abl alb > 0), we obtainT abl alb > 0 . We briefly review how the entropy increase theorem can be established in the Einstein frame from the above null Raychaudhuri equation (58). The process is similar to standard GR. The entropy of a black hole in the Einstein frame isS =Ã/4 [21,22,56], whereÃ is the surface area of the null horizon of the black hole.Ã can also be written asÃ whereq is the determinant of the induced metricq ab . Now, it can be shown that Using (60) one can obtain the change of entropy along λ a (i.e. £lS = dS/dλ) as Therefore, the entropy can only decrease (i.e. dS/dλ < 0) whenθ is negative. However, if the formation of caustics is prohibited, then from the Raychaudhuri equation (58) one finds thatθ cannot be negative, taking in to account the null energy condition, i.e.T abl alb > 0. From this argument one finds that the entropy must always increase.

B. Jordan frame
We now repeat the same analysis in the Jordan frame. In the Jordan frame, Bekenstein's formula for entropy breaks down since the entropy now is proportional not only to the area of the horizon, but is also proportional to the scalar field φ, as suggested by Kang [57] (also see our previous work [21,22], where the same result was shown via different means). Thus the expression for the entropy, S, in the Jordan frame is Therefore, the rate of change in entropy is Thus, even in the Jordan frame, it isθ and not θ that determines whether the entropy should increase. This is because, as we have discussed earlier [21,22], thermodynamically the two frames are equivalent. Therefore, the appropriate Raychaudhuri equation, which is consistent with the thermodynamic description, should be defined in terms of those quantities (i.e. shear, expansion scalar and energy-momentum tensor) which were obtained in the equivalent picture of the fluid-gravity dual description. From (58), one can obtain the expression for the Raycharudhuri equation in terms of the parameters in the Jordan frame as whereT ab =Tφ ab + (T ext ab /φ) . To obtain the above equation, we have used dθ/dλ =l a ∂ aθ = l a ∂ aθ = dθ/dλ . We again note thatTφ ab l a l b = (l a ∂ aφ ) 2 ≥ 0. Therefore, when the external matter field satisfies the null energy condition (i.e. T ext ab l a l b > 0), we obtainT ab l a l b > 0 . Then following the arguments as in the Einstein frame, one can prove thatθ is always positive, which proves the entropy increase theorem in the Jordan frame.
In this section we have found that it isθ which comes into play in obtaining the entropy increase theorem in the Jordan frame. This is consistent with the fact that the two frames are thermodynamically equivalent. In addition, we have obtained the null Raychaudhuri equation in each frame which is consistent with the thermodynamic description in scalar-tensor theory.

V. TIDAL FORCE EQUATION
The Raychaudhuri equation discussed in the previous section describes how the trace part of θ ab orθ ab (i.e. θ orθ) evolves in the spacetime. On the other hand, the tidal force equation describes the evolution of the traceless part of θ ab orθ ab (i.e. σ ab orσ ab ) [24]. In this section, we shall discuss the expression of the tidal force in the two frames. In obtaining the tidal force equation, the equation of motion is not used. Therefore, the standard expression for the tidal force equation from GR is also valid for scalar tensor theory.
In our equivalent fluid-gravity dual description, it is Σ ab (and not σ ab ) which we have identified as the shear tensor in the Jordan frame. Σ ab is also conformally invariant, since Σ ab =σ ab . Thus, in the Jordan frame, we have to examine how Σ ab evolves in the spacetime. The standard expression of the tidal force equation [24,25] valid in the Einstein frame, is given bỹ whereC abcd is the Weyl tensor -the traceless part of the Riemann tensorR abcd . The explicit form ofC abcd is where n is the dimension of the whole manifold. The RHS of (65) gives the measure of the tidal force on the two-surface S t . We now obtain the the tidal force equation in the Jordan frame. Using the conformal transformation (4) and (5) we can obtain, from (65), The above form of the tidal force equation is consistent with the equivalent fluid-gravity picture. However, the usual the tidal force equation of GR is consistent with the inequivalent fluid-gravity picture. In this case, the expression of tidal force equation is

VI. SUMMARY AND CONCLUSIONS
The connection of the field equation of the gravity with fluid dynamics (i.e. that the Einstein equation can be identified with the Navier-Stokes equation by projecting the GR equation onto a null surface) is a remarkable discovery due to Damour [23] . Later, this fluid-gravity connection was established in several ways  and this connection is now considered as a remarkable feature of general relativity. Over the last few decades, several alternative theories of gravity have developed as extensions/substitutions of GR. The question, which motivated the analysis in this paper, was whether the fluidgravity connection is a special characteristic of standard GR only, or can one obtain a similar connection for these alternative gravity theories. Also it is of interest to determine how the expressions of the fluid parameters in these alternative gravity theories look, and to what extent they differ from standard GR. In this work, we have obtained the fluid-gravity analogy in the scalar-tensor theory of gravity, which is one of the most promising theories among various alternative theories of gravity. Moreover, since any f (R) gravity theory can be written in terms of a corresponding scalar-tensor theory, this work implies that the present analysis is relevant for establishing the fluid-gravity correspondence in higher curvature gravity theories. In addition, scalar-tensor theory is described in both the Jordan frame and the Einstein frame. These two frames are conformally connected to each other. The physical equivalence of these two conformally connected frames has been a matter of debate for several decades. From the thermodynamic viewpoint, the two frames are physically equivalent. However, from the fluid-gravity viewpoint the above analysis shows that no definite conclusion can drawn in this regard.
In this paper we first provided a brief overview of the scalar-tensor theory of gravity in both the Jordan and Einstein frames. Second, we briefly described the geometry of the null-surface in the context of (1 + 3) spacetime foliation, an idea which is necessary in order to obtain the projected form of the gravitational field equation onto the null surface. Then, we obtained the DNS equation in the Einstein frame, following a similar approach to that used in standard GR. We found that the complete form of the DNS equation could be obtained even without considering the external matter field, unlike the case in standard GR. Later we showed that one cannot obtain the DNS equation in the Jordan frame by following the same procedure as in standard GR. In particular, in the Jordan frame, one finds that there are two different cases to get the DNS equation. In the first case, we have shown that one can obtain the DNS equation along with an additional Coriolis-like force term. This picture is consistent with some recent work in the framework of f (R) gravity. Moreover, in this first case, the ratio η/s saturates the KSS bound. However, in this case, the fluid parameters are not equivalent to those of the Einstein frame. Later, we showed that an equivalent case is also possible in the Jordan frame. In this second case the DNS equation can be obtained in terms of fluid variables, which are equivalent to those of the Einstein frame. In this method, the Coriolis-like force term does not appear in the DNS equation. However, as we have mentioned earlier, the equivalent picture is less favoured by the KSS bound, since this bound is violated in this case. We believe, more investigation is required in this regard to provide any definite conclusion.
After obtaining the DNS equation in the Einstein and Jordan frames, we discussed the Raychaudhuri equation in the two frames in the context of the generalized second law. As shown in this work, the second law of thermodynamics can be obtained from the Raychaudhuri equation. However, in the Jordan frame, the evolution of the expansion scalar θ does not determine the entropy increase theorem, but rather it is determined byθ. Therefore, we identify the proper Raychaudhuri equation as the evolution ofθ in the Jordan frame. Finally, we showed how the shear tensor evolves in the spacetime by obtaining the tidal force equation in the two frames. We mentioned how the tidal force equation of standard GR continues to be valid for the Einstein frame of ST gravity. The same expression of the tidal equation is also consistent with our inequivalent picture of the fluid-gravity duality in the Jordan frame. Additionally, we also obtained the tidal force equation which is consistent with the second (equivalent) case of the fluid-dynamic description in the Jordan frame.
The analysis in this paper indicates that the fluid-gravity correspondence is a general characteristic of gravity theories, similar to the correspondence between thermodynamics and gravity. This connection with fluid dynamics is not limited to standard GR. In the present case, we have shown that this correspondence with fluid dynamics also works with scalar-tensor gravity. This connection between fluid dynamics and scalar-tensor theory, also implies that this correspondence exists for f (R) gravity, since f (R) gravity can be described as a scalar-tensor gravity. Our analysis also suggests that, unlike the thermodynamic case, where the two frames are exactly equivalent, from the fluid-gravity perspective it is possible to obtain both equivalent as well as inequivalent cases. For the time being, we can say that the inequivalent case is consistent with the KSS bound saturation which has been predicted to hold in f (R) gravity from and AdS/CFT viewpoint [53]. The present analysis should be useful in the context of the fluid-gravity analogy and also in the theory of scalar-tensor gravity.