Thermal entropy of a quarkantiquark pair above and below deconfinement from a dynamical holographic QCD model
Abstract
We discuss the entropy carried by a quarkantiquark pair, in particular across the deconfinement transition. We therefore rely on a selfconsistent solution to EinsteinMaxwelldilaton gravity, capable of mimicking essential features of QCD. In particular we introduce a novel model that still captures well the QCD confinement and deconfinement phases, while allowing the introduction of a temperature in a phase which resembles the confined phase, this thanks to it being dual to a small black hole. We pay due attention to some subtleties of such model. We confirm the lattice picture of a strong buildup of thermal entropy towards the critical temperature , both coming from below or above . We also include a chemical potential, confirming this entropic picture and we consider its effect on the speed of sound. Moreover, the temperature dependent confinement phase from the holography side allows us to find a string tension that does not vanish at , a finding also supported by lattice QCD.
1 Introduction
The investigation of QCD at finite temperature is extremely important for various reasons, ranging from heavy ion physics to cosmology. It is expected that studies of heavy quarkonium at finite temperature may enhance our understanding of the deconfinement transition and that these may shed new light onto the (creation of the) QCD plasma phase. A lot of new results, both from experimental as well as from theoretical side, are appearing. For example, recent experimental results from RHIC and LHC have indicated a strong suppression of charmonium near the deconfinement transition [1, 2]. The nontrivial experimental result that the charmonium suppression is stronger at lower energy density than at larger energy density has led to an intense investigation into the nature of this suppression and many theoretical scenarios such as the renown colour screening mechanism [3], a recombination of the produced charm quarks into charmonia [4, 5], the imaginary potential mechanism for heavy quark dissociation [6, 7, 8], etc have been suggested for its explanation.
One such mechanism which attracted interest of late, and a topic of this paper, was proposed in [9]: it was suggested that the suppressed production of heavy quarkonium may be related to the nature of the deconfinement transition. In [9], based on lattice QCD results [10, 11, 12], the notion of an “emergent entropic force”,
was introduced. Here denotes the entropy, is the temperature and is the interquark separation. The lattice prediction that the entropy of a quarkantiquark () pair increases with distance, shown in Figure 2, leads to a positive repulsive force and can promote the selfdestruction of the bound state. It was shown that the destruction of a bound state to a delocalized state was maximal near the deconfinement transition temperature, giving a possible explanation for the strong suppression of quarkonium around that temperature.
The emergent entropic force mechanism of [9] is thus based on lattice QCD simulations which suggested a considerable amount of entropy is associated with a pair in the hot QCD plasma, indicating a strong entanglement between the heavy bound states with the rest of QCD plasma. The lattice QCD data are summarized in Figures 2 and 2. Some of the main lattice observations are i) prediction of a large amount of entropy associated with a heavy pair near the deconfinement transition temperature ii) away from the deconfinement temperature the entropy decreases with temperature in both confined and deconfined phases and iii) the entropy grows as the separation between the quarks increases. This entropy first increases gradually and then saturates to a constant value at large separations.
As emphasized in [13, 14], the lattice data for the entropy at the peak near the transition temperature also indicates the breakdown of the weak coupling approximation. The entropy near the transition temperature computed from a mean field Debye screening approximation was found to be an order of magnitude lower than that of lattice results. This suggests the need of a method which is more suitable for entropy calculations in the strongly coupled regime. One such nonperturbative method is the gauge/gravity duality [15, 16, 17]. Using this duality, a lot of new insights into the regime of strongly coupled QCD, which agrees qualitatively with the lattice QCD results, have been obtained both from “topdown” and phenomenological “bottomup” models [18, 19, 20, 21, 22, 23, 24, 25, 26, 27, 28, 29, 30, 31, 32, 33, 34, 35, 36, 37, 38, 39, 40, 41, 42, 43]. Since gauge/gravity duality provides a valuable and unique technique to investigate strongly coupled gauge theory, therefore it would be interesting to see whether this duality can also provide new insights into the entropy of the pair.
The entropy of the pair and the idea of an entropic force was first discussed holographically in [14] for topdown models. Two models — supersymmetric YangMills theory (SYM) and Pure 4D YangMills theory obtained from compactification of 5D SYM on a circle— were considered and the holographic thermal entropy was calculated from the free energy of an open string hanging from the asymptotic boundary into the bulk spacetime [44, 45, 46]. Albeit not exactly corresponding to the (lattice) QCD setup, similar features were seen in these dual black hole phases: the growth of the entropy with interquark distance, saturation to a constant value at large separations and in the second case, a divergence at the deconfinement temperature, reflecting the sharp peak observed in genuine lattice QCD. These calculations were then extended to other holographic models in [47, 48, 49]. However, since these two holographic models do not accurately describe real QCD, there were some discrepancies too. For example, the higher temperature asymptotics of the entropy do not reconcile with lattice QCD results. This discrepancy was later rectified in [47] using the improved holographic bottomup models of [26, 27]. Another important lattice result which could not be reproduced by holographic models in [14, 47] was the temperature dependence of the entropy in the confined phase. This is precisely due to the fact that in the gauge/gravity duality, the confined phase is generally dual to an asymptotically AdS space (without a horizon), which is thence independent of temperature. Subsequently all the physical quantities in the confined phase are independent of temperature. In order to study temperature dependence in this phase one would need to consider corrections in the holographic models, something extremely difficult to calculate.
However there might be another way to introduce temperature dependence in the confined phase, without having to compute corrections: we can construct a black hole solution whose dual boundary theory satisfies all the necessary properties of confinement. By confinement we simply mean a phase that satisfies area law behaviour for the (expectation value of the) Wilson loop and a Polyakov loop with vanishing expectation value ^{1}^{1}1We work in the holographic analogue of quenched QCD, i.e. with nonpropagating quark flavour degrees of freedom. As such, QCD enjoys an explicit symmetry in the confined phase, with the Polyakov loop expectation value serving as order parameter.. Indeed, one can see from Figure 2 that even in the confined phase a large amount of entropy is associated with the pair and therefore it is important to try to analyze this observation from the holography viewpoint. The black hole solution will naturally introduce a notion of temperature in the confined phase and it would be interesting to see whether such solution, if constructed, can also capture lattice results for the entropy of the pair. We will show in section 3 that it is indeed possible to construct such a close cousin of the confined phase, which we call speciousconfined phase, for which the dual gravity side contains a black hole. Interestingly, the entropy of the pair in this holographic speciousconfined phase turns out to be in qualitative agreement with lattice QCD confined phase results. The speciousconfined model will also allow us to study, to our knowledge for the first time from holography, the temperature dependence of the ensuing QCD string tension, finding qualitative agreement with quenched lattice QCD as well, in the sense that the string tension does not vanish at deconfinement [50, 51, 52].
It is also well known that the QCD phase diagram strongly depends on the chemical potential (i.e. a nonzero quark density). In particular, the confinement/deconfinement transition temperature and QCD equation of state are sensitive to the value of the chemical potential. Accordingly, one might think that the entropy of the pair may also depend nontrivially on it. However such results are are not available in lattice QCD yet due to the sign problem plaguing finite density simulations. In the absence of lattice QCD results, therefore, it is of great importance to investigate the entropy holographically and see the effects of chemical potential on it.
In this work our aim is to construct one such holographic QCD model that displays qualitative agreement with lattice results for the entropy, not only for the deconfined phase but in particular for the confined phase as well. We will also include effects of a chemical potential. For this purpose we consider a phenomenological bottomup EinsteinMaxwelldilaton gravity model [53, 54, 55, 56, 57, 58, 59, 60, 61, 62, 63]. The gravity system is analytically solvable in terms of an arbitrary scale function (see eq. (2.14)), depending on which there can be various kinds of phase transitions on the gravity side. In this paper, we consider two different forms for . The first form, discussed in eqs. (3.1), leads to a first order phase transition in terms of a small to a large black hole phase. These small and large black hole phases correspond to speciousconfinement and deconfinement phases in the dual boundary theory respectively. Notably, the boundary dual of the small black hole phase does not exactly correspond to confinement as it has a nonzero (albeit exponentially small) Polyakov loop expectation value while showing linear confinement for larger distances at low temperatures only. For this reason we called this dual phase speciousconfined instead of confined. Furthermore, the speciousconfinement/deconfinement transition temperature decreases with the chemical potential and the corresponding first order small/large black hole phase transition line terminates at a second order critical point, as predicted by the wellknown lattice study [64]. Similarly, the second form of , shown in eqs. (4.1), leads to a first order Hawking/Page phase transition from thermalAdS to black hole on the gravity side. These thermalAdS/black hole phases correspond to the standard confinement/deconfinement phases in the dual boundary QCD theory.
Having constructed a black hole solution (using the first form of ) for both speciousconfinement and deconfinement phases, we then study temperature dependence of the entropy in these phases. We find that our phenomenological model does qualitatively reproduce the lattice QCD results of the entropy. Our main results are shown in Figures 13, 13 and 15. In the deconfined phase, we find that our gravity model displays the growth of the entropy with interquark distance, corroborating the entropic force scenario of [9] for the selfdestruction of the bound state. This entropy saturates to a constant value at large distances, as also predicted by lattice QCD. Our model further reproduces a sharp peak in the entropy near the critical temperature. The sharp peak near the critical temperature can be appreciated from both deconfined as well as from speciousconfined phases. Interestingly, even though speciousconfined is strictly speaking not referring to a genuine confined phase, the entropy of the pair matches qualitatively with the lattice QCD predictions. We further provide a holographic estimate for the entropy with chemical potential which could be tested using lattice QCD in the near future. Similarly, the results for the entropy using the second form of are again in agreement with lattice QCD. The qualitative results in the deconfined phase remains the same, however, since the confined phase is now dual to thermalAdS, the entropy is zero in that phase.
We also study the speed of sound () in our holographic models and find results which again are in qualitative agreement with lattice QCD. In particular, as in lattice QCD, is greatly suppressed near the transition temperature in both models. Importantly, is suppressed in the speciousconfined phase side too. We find that approaches its conformal value from below at high temperatures. Our results further indicate that higher values of chemical potential try to suppress more near the transition temperature. However for extremely low (in the speciousconfined phase) and high temperatures, approaches a chemical potential independent constant value.
The paper is organized as follows. In the next section, we describe our gravity model and obtain the solution analytically. In section 3, using a particular form of , we first study the thermodynamics of the gravity solution and then discuss the free energy and entropy of a pair with and compare it with lattice QCD results. We repeat the calculations of section 3 with a different Ansatz in section 4. In section 5, we study the speed of sound in the constructed speciousconfined, confined and deconfined phases. Finally, we conclude this paper with some discussions and an outlook to future research in section 6.
2 EinsteinMaxwelldilaton gravity
We start with the EinsteinMaxwelldilaton action in five dimensions,
(2.1) 
where is the corresponding Newton constant, is the potential of the dilaton field and is a gauge kinetic function which represents the coupling between dilaton and gauge field . The Einstein, Maxwell and dilaton equations of motion derived from eq. (2.1) are, respectively,
(2.2) 
(2.3) 
(2.4) 
where
In order to simultaneously solve eqs. (2.2), (2.3) and (2.4), we consider the following Ansätze for metric, gauge and dilaton fields,
(2.5) 
where we have assumed that the various fields depend only on the extra radial coordinate . Here is the AdS length scale and in our notation, corresponds to the asymptotic boundary of the spacetime, i.e. where the strongly coupled gauge theories is located.
Plugging the above Ansätze into eqs. (2.2)(2.4), we get the following equations
(2.6) 
(2.7) 
(2.8) 
(2.9) 
(2.10) 
where only four of the above five equations are independent. In the following, we treat eq. (2.6) as a constraint equation and consider eqs. (2.7)(2.10) as independent equations. Importantly, these independent equations can be solved analytically in term of functions and i.e. in terms of a scaling factor and a kinetic gauge function [60, 61]. In term of and , the solutions are
(2.11) 
where we have used the boundary condition that at the horizon and goes to 1 at the asymptotic boundary. It can be explicitly verified, with the help of the potential expression in eq. (2.11), that the Einstein, Maxwell and dilaton equations are indeed satisfied. The undetermined integration constant in eq. (2.11) can be fixed in terms of a chemical potential () present in the boundary theory. Expanding near the asymptotic boundary and using the gauge/gravity mapping, we get
(2.12) 
The only nontrivial inputs which remain to be fixed are and . Indeed eq. (2.11) is a gravity solution for the EinsteinMaxwelldilaton system for any and . Therefore, we have a freedom of choosing any and . We can use this freedom to constrain the arbitrary factors and by matching the properties of the boundary gauge theory with real QCD. For example, can be fixed by demanding the dual boundary theory to satisfy linear Regge trajectories, i.e. the squared mass of the mesons vary linearly with respect to the radial excitation number. In this paper, we will consider the following simple form for
(2.13) 
Using this form of , one can easily show that the discrete spectrum of the mesons indeed lie on a linear Regge trajectory. One can fix the magnitude of by matching the holographic meson mass spectrum to that of lowest lying heavy meson states [60]. By doing that, one gets ^{2}^{2}2The factor can also be fixed by matching with the meson mass instead, as done in e.g. [65]. However, since we are more interested in the properties of heavy bound states, we find it more appropriate to compare with the and state, following [60].
With this choice of , the gravity solution is then given by
(2.14) 
where
We now have a complete solution of EinsteinMaxwelldilaton gravity system. The solution in eq. (2.14) corresponds to a black hole with horizon at . The Hawking temperature and entropy of this black hole solution are given by,
(2.15) 
Let us also mention that there is another solution to the EinsteinMaxwelldilaton equations, i.e. one without a horizon corresponding to a thermalAdS space. The thermalAdS solution can be obtained by taking the limit of the black hole solution presented above, i.e. . Although this thermal solution again asymptotes to AdS at the boundary, however depending on the scale factor , it can have a nontrivial structure in the bulk. This solution will play a significant role in our analysis in section 4.
The only function that now remains to be fixed is the scale factor . Indeed, in order to proceed further we now need to specify a specific form for . In the next two sections, we consider two different forms of and study the thermodynamics of the gravity system, the free energy and entropy of the pair, speed of sound etc for each form separately. As we will show, depending on the form of , there can be various kinds of phase transitions between the gravity solutions, and correspondingly, the interpretation of these gravity solutions in the boundary gauge theory can be different.
Above we have presented a gravity solution in the Einstein frame, useful for investigating thermodynamical properties and equations of state of the system. However, in order to study some confinement/deconfinement properties and in particular the free energy of a pair, it is more convenient to use the string frame metric. It can be obtained from the Einstein frame metric by the following standard transformation via the dilaton,
(2.16) 
where .
For completeness, we should mention here that we treat the scalar field as a genuine dilaton, although our models are lacking, as any bottomup AdS/QCD model, a proper embedding into an underlying string theory. If was just another scalar field other than a dilaton ^{3}^{3}3See for example [66, 67, 68] exploring this possibility. so that , then confinement and all of its related features are absent and thus any qualitative comparing with QCD becomes obsolete, both from the Case 1 and Case 2 model we are going to discuss below. This finding is analogous to another selfconsistent model used to connect to magnetized QCD, as introduced and discussed in [69].
Before ending this section, we like to mention that the Gubser criterion of [70] for Einsteinscalar gravity theory is satisfied in our gravity model as well ^{4}^{4}4Other, stronger, criteria for the physical reliability of generic naked singularities are suggested in [68, 71], but our potentials fall beyond the class discussed there.. More precisely, the dilaton potential at any point in the bulk is bounded from above by its value at the UV boundary, i.e. .
3 Case 1: specious confinement
Let us first consider the following simple form of ,
(3.1) 
It is straightforward to see that at the boundary . This is nothing but the statement that bulk spacetime asymptotes to AdS at the boundary. Moreover, expanding the dilaton field and potential near the asymptotic boundary and rewriting the dilaton potential in terms of dilaton field, we get
(3.2) 
The above equation indicates that the dilaton mass meets a well known result in gauge/gravity duality, i.e. . The dimension of the dual operator satisfies the BreitenlohnerFreedman (BF) bound as well [72, 73]. Furthermore, near the boundary we have , where is the negative cosmological constant in five dimensions, as expected.
The parameters and in can be determined by comparing the holographic results with lattice QCD results at zero chemical potential. For example, as we will show shortly, the gravity solution with the above form of undergoes a small to large black hole phase transition. This phase transition has been suggested to be dual to confinementdeconfinement phase transition in the boundary side [60, 61]. Demanding the critical temperature of this transition at zero chemical potential to be around ^{5}^{5}5See [74] for a lattice determination of the deconfinement temperature for pure gauge theories for several values of . Only a mild dependence on (growing) is to be reported. fixes the parameters and as
We again like to emphasize that eq. (2.14) is a solution of EinsteinMaxwelldilaton system for any , and eq. (3.1) is just a particular form. We chose this expression to reproduce some of the QCD results holographically, after which new predictions for other quantities can be made without further introduction of new parameters.
3.1 Black hole thermodynamics
Let us first discuss the thermodynamics of the gravity system with as in eq. (3.1). All the results in this section should be understood to be derived from this form of .
The variation of Hawking temperature with respect to horizon radius for various values of chemical potential is shown in Figure 4. We find that for small chemical potential there are three branches in the plane, out of which one branch is stable, one metastable and the last branch is unstable. The stable and metastable branches, for which the slope in plane is negative, correspond to small and large black hole phases. For the unstable branch, the slope is positive. This suggest a phase transition form a small black hole (large ) to a large black hole (small ) as we steadily increase the Hawking temperature. This is indeed the case as can be observed from the free energy behaviour which is shown in Figure 4. In Figure 4, we used the normalization such that the free energy of thermalAdS is zero. We see that the free energy has a swallowtail like structure — a characteristic feature of a first order phase transition — for small chemical potential. The unstable branch corresponds to the base of the swallowtail and a phase transition occurs at the kink. The corresponding temperature at the kink around which the free energy of the large black hole becomes larger than that of the small black hole defines the critical temperature . For , we find . Importantly, the free energy is always negative in stable branches which indicates that the black hole phase always has a lower free energy than thermalAdS and hence is more stable.
However, the above pattern changes as we increase the value of . For higher values of , the size of the swallowtail starts to decrease and it completely disappears above a certain critical chemical potential . For , we find . At , the large and small black hole branches merge together and form a single stable black hole branch which is stable at all temperature. This can be seen from cyan curve for which is considered. The overall dependence of on is shown in Figure 5. We find that decreases with . The solid line in Figure 5 which separates the small and large black hole phases terminates at the second order critical point. This behaviour is analogous to the Van der Waal like liquidgas phase transition and has been thoroughly discussed in context of charged AdS black holes in many cases [75, 76, 77, 78, 79, 80].
The above smalllarge black hole phase transition on the gravity side has been suggested to correspond to the confinementdeconfinement phase transition in the dual boundary side in [60, 61] ^{6}^{6}6In [60, 61], a different expression for was used.. In particular, the small black hole phase was suggested to be dual to confinement whereas the large black hole phase was suggested to be dual to deconfinement. However, as we will show shortly, this interpretation is not entirely correct. Especially, there are a few nontrivial issues in interpreting the small black hole phase as dual to confinement. Again by confinement we simply mean a phase for which the Wilson loop expectation value satisfies the area law while the expectation value of the Polyakov loop is zero. We will show in the next section that by taking the correct expression of the free energy neither of these conditions are strictly satisfied in the boundary theory dual to the small black hole phase. However interestingly, despite of these limitations in interpreting the small black hole phase as being dual to genuine confinement, the entropy of the pair and speed of sound in this phase turn out to be in good qualitative agreement with lattice QCD in its confined phase.
3.2 Free energy of the pair
In order to study the Wilson and Polyakov loops, we first need to access the free energy of a pair which can be easily computed holographically from the world sheet onshell action.
The gauge/gravity correspondence relates the free energy of a pair to the onshell action of a fundamental string in the dual gravity background. In particular, the of a pair separated by a distance and evolving over time can be calculated by the onshell action of the fundamental string, with the boundary condition that at the asymptotically AdS boundary, the string world sheet shares the rectangular boundary of sides and . We have
(3.3) 
where is the temperature and is the open string onshell NambuGoto action,
(3.4) 
Here, denotes the gravity background in string frame ^{7}^{7}7In the following, a subscript “” is used to denote quantities in the string frame., denote the open string embedding, is the open string tension and are the world sheet coordinates. Depending upon on the background geometry there can be multiple open string solutions and below we will show that each solution provides a unique result which can mimic the results of lattice QCD.
Here we will work in the static gauge with and . In this case there can be two world sheet configurations that minimize the NambuGoto action: a connected and a disconnected one. The connected world sheet is a shape configuration which extends from the boundary () into the bulk. In this case, we have the following expression for the free energy of the pair
(3.5) 
where is the turning point of the connected world sheet. This turning point is related to the length of the pair as
(3.6) 
On the other hand, the disconnected configuration consists of two lines which are separated by distance and are extended from the boundary to the horizon,
(3.7) 
is independent of and therefore of the separation length as well. Here, for the black background and for thermalAdS. It is important to mention that both and are divergent quantities. The divergence arises from the part of the integral. In order to regularize the free energy, we will use the temperature independent renormalization scheme suggested in [81], which amounts to minimally subtracting the pole when cutting at the integral at . However, in most part of this paper we will deal with the difference in free energy anyhow where the diverging parts trivially cancel out.
Let us first consider the large black hole phase (small ) as a gravity background. In Figure 7, the length as a function of for various values of the horizon radius is plotted. We observe that for every horizon radius there exists an above which the connected string configuration does not exist. We further find that there are two solutions for a given : one for small (solid lines) and one for large (dotted lines). As we will see shortly, the one with smaller corresponds to an actual minimum of the string action whereas the one with larger corresponds to a saddle point.
In Figure 7, we have shown the difference in free energy between the connected and disconnected string solutions. In this Figure, solid and dotted lines correspond to smaller and larger branches of respectively. We observe that the former branch always has a lower free energy than the latter branch, indicating that it is a true minimum. However, we also observe that can be greater or less than zero depending on the value of . This suggests a phase transition from a connected to a disconnected string solution as we increase the (QCD) string length . The string length at which turns from negative to positive value defines the critical length . We find that increases with increasing . This suggests that for larger size black holes (small ), the connected string configuration confines closer to the AdS boundary. The behaviour that decreases with temperature is consistent with the physical expectation that at higher and higher temperatures the boundary meson state would eventually melt to a free quark and antiquark (deconfined phase), a situation which is on the dual gravity side described by the disconnected string configuration. Since for large separations, this disconnected string configuration which is independent of separation length is more favourable, therefore the corresponding free energy of the pair is also independent of . It implies that the QCD string tension is zero and that there is no linear law confinement in the boundary theory dual to the large black hole phase.
We now discuss the free energy of a pair in the small black hole phase (large ). We find that for a small black hole background, does not exist and continuously increases with . This is shown in Figure 9. The string world sheet does not penetrate deep into the bulk and saturates near , suggesting some kind of an “imaginary wall” in the bulk AdS which cannot be penetrated by the string world sheet. Around this wall, also increases rapidly. At first sight this naively suggests that in the small black hole background, the pair is always connected by an open string and forms a confined state. However, we need to be careful with this interpretation as we will show shortly. The regularized part of the corresponding free energy curve is shown in Figure 9. We find that is negative for small and increases linearly for large . In fact, it can be shown analytically that for small exhibiting a Coulomb potential, and for large suggesting confinement [60]. Here is the QCD string tension. Therefore, from the connected string configuration in the small black hole background we get the famous Cornell expression [82]
for the energy of a pair. By comparing the lattice QCD estimate of the string tension, [83], with our numerical results, we can further fix the value of the open string tension in units of the AdS length scale . By doing that we find . This small value of , corresponding to a small ’t Hooft coupling, generally indicates the breakdown of the classical gravity approximation and it suggests that the higher derivative correction terms might become important. Although the small value of is certainly a drawback of our model, however, we also like to point out that most of the phenomenological bottomup gauge/gravity models suffer from this ambiguity (see for example [58], based on the selfconsistent model of [53, 54] or [84, 85], to name only a few.), and other models which do exhibit a large generally have additional scaling symmetries in the dilaton potential (or additional parameters) which makes a large arguable as it depends nontrivially on those additional scaling (as well as on the choice of dilaton normalization) [30]. See [66] for further details on certain conceptual difficulties associated with the magnitude of in bottomup holographic models. Clearly it is an unsettled relevant question and more work is needed. Currently we do not have a resolution for this problem. Indeed, the size of is only determined quantitatively upon selecting a “stringy” (loop related) QCD observable. In practice, this is usually achieved by matching on the string tension entering the Wilson loop, or, in the presence of dynamical quarks, the Polyakovloop related free energy. If we refrain from matching to the precise QCD values, our qualitative findings stand as they are and are trustworthy. Keeping this ambiguity in mind, in the current work we will always express the free energy and entropy of the quark pair in (unspecified) units of . This is reasonable as our main aim here is to find a qualitative picture for the free energy and entropy of the quark pair from holography. Such approach is not uncommon, notice that also in [32] thermodynamics of unquenched holographic QCD was discussed without actually fixing the string tension. Though, it must be kept in mind that quantitative holographic QCD looprelated results will only be trustworthy at the expense of having these quantities an order of magnitude smaller than expected from comparing with genuine QCD.
It is clear from the linear dependence of on the interquark separation length that the Wilson loop of the dual boundary theory exhibits an area law, as one expects for a confined gauge theory, and that the boundary theory dual to the small black hole phase seems to satisfy the typical properties of confinement. This behaviour of was used in [60, 61] to motivate that the small black hole phase is actually dual to confinement.
However, as mentioned before, we need to be careful with the above interpretation. In particular, the connected string is not the only world sheet solution of the NambuGoto action and one needs to compare with the free energy of the disconnected string as well. Generally, in the gauge/gravity correspondence, the confined phase is dual to a thermalAdS space. In that case the upper limit in the integral of is at , which makes divergent. Therefore, in that case the connected string always gives a lower free energy than the disconnected one. Consequently, one gets a linear law confinement for the pair from the connected string solution using the dual thermalAdS background. However, with a black hole background, the disconnected strings extend from the asymptotic boundary to maximally the horizon at , which makes finite (of course after removing the usual UV divergences), and hence its free energy could become less than as well. For this reason, it is now important to compare and when one uses black hole backgrounds (like we did in the large black hole phase in Figure 7) to get the true minimum of NambuGoto action and correspondingly to study the properties of confinement and deconfinement.
The comparison between and in the small black hole background is shown in Figure 11, where is plotted as a function of for the same parameter values as in Figure 9. We see that can indeed be greater than zero, especially for large separation length. This implies that is actually the true minimum for the string action for large , and therefore, one should consider to study the (correct) properties of the pair. Accordingly, since is independent of , the string tension is zero and hence there is no more linear law confinement in the boundary theory dual to small black hole phase. Therefore, although does indeed show an area law for the Wilson loop, however, it is that is relevant for large , not leading to an area law. Further details are presented in Figure 11, where flattening of interquark energy at large is explicitly shown.
In Figure 11, the behaviour of the free energy as a function of for various temperatures is shown. For (lines above the upper black line), we are in the small black hole phase; and for , (lines below the 2nd black line), we are in the large black hole phase. The two black lines correspond to at which the small and the large black hole phases (having different horizon radius) coexist. We find that the string tension for , calculated from the slope of the linear part of , is almost temperatureindependent and remains nonzero even at , a result supported by lattice QCD as well [50, 51]. Moreover, for the size of the linear part in starts to decrease and so is the string tension. However, as opposed to its lattice QCD counterpart, there exists a small discontinuity in the string tension at . This can again be traced back to the first order phase transition between the small and large black hole phases at , where both phases coexist.
For completeness, let us notice that according to Figure 11, the critical length at which the string tension vanishes in the speciousconfined phase, decreases with increasing temperature. A similar signal is obtained from the entanglement entropy using the same model [86].
To appreciate the length scales in Figure 11, let us remind here the typical scale of heavy quark bound states, like charmonia, having a binding size of the order of [87]. In [51], the linear potential at was considered up to . ^{8}^{8}8 is the string tension at . This strongly suggests that the values of obtained here for temperatures not too far from , are well compatible with QCD phenomenologically relevant length scales.
We further like to add that these results are valid irrespective of the value of the chemical potential. For example, for finite we again find for large . Moreover, at a fixed temperature, is found to decrease with in the small black hole phase.
Further evidence for the problem of correctly interpreting the small black hole phase as the gravity dual of confined phase can be inferred from the Polyakov loop expectation value. As said before, and well known in the literature, the Polyakov loop acts as an order parameter for the confinement/deconfinement phase transition, vanishing in the confined phase and attaining a nonzero value in the deconfined phase. Therefore it is of importance to find out how the expectation value of Polyakov loop behaves in the current model.
The expectation value of the Polyakov loop can be calculated holographically from the heavy quark free energy. The regularized form of the latter (after removing the UV divergence) is given by
(3.8) 
from which one can extract the Polyakov loop
We see that can be zero in confined phase when either is zero or is divergent. In the small black hole phase, none of these conditions is met. For example, is finite for the small black hole phase and, as discussed above, does not have an IR divergence. Therefore, the Polyakov loop expectation value is strictly nonzero for the boundary theory dual to the small black hole phase and consequently this dual boundary phase is not exactly corresponding to a confined phase.
We have followed the holograpic literature here and considered a single Polyakov loop, even in the presence of a nonvanishing chemical potential [57, 32, 88]. We should however notice that the latter breaks the charge conjugation symmetry C between the (unequal number of) quarks and antiquarks, and as such the Polyakov loop expectation values for an isolated quark or antiquark are not supposed to be equal [89, 90, 91]. In the current approximation of the gaugegravity duality to access loop quantities as the Polyakov loop, we are however unable to probe this C breaking since the NambuGoto action is blind to . It would require to take into account stringy corrections to the classical NambuGoto worldsheet action (including back reaction corrections related to introducing either a quark or antiquark located at the end point of the string considered dual to the loop), a task far beyond this and most –not to say all– other works on holographic QCD models.
We also like to point out another important issue here. Although, is nonzero in the small black hole phase in a strict sense, however it is extremely small. For instance, at , and its magnitude is even smaller at lower temperatures. Moreover, it is also clear from Figure 11 that the value of at which changes its sign, increases with decreasing temperature (or as increases). This suggest that for smaller and smaller temperature, the quark and antiquark form a bound state up to larger distances. For example, at is an order of magnitude larger than at . For these reasons, keeping in mind various technical issues in interpreting the small black hole phase as the gravity dual of the confined phase, we may call this dual phase the speciousconfined phase, to distinguish it from the “standard” confined phase. We will see in the following sections that the entropy of the pair as well as the speed of sound in this speciousconfined phase is also rather similar to that of the lattice QCD confined phase.
Strangely, our speciousconfined phase resembles the behaviour of full (unquenched) QCD at the level of nonlocal observables such as Wilson or Polyakov loops expectation values, while at the level of thermodynamics, it becomes closer to quenched QCD. In full QCD, the Polyakov loop is not an exact order parameter because of the explicit breaking of the symmetry due to the dynamical quarks in the fundamental representation. Moreover, quark pair creation prevents the linear behaviour of the confining potential in full QCD, rather one observes a flattening (the socalled “string breaking”) at larger values of [92], not unlike what we find here. Indeed, as shown in Figure 11, one can clearly observe the flattening of interquark energy for large . Moreover, just like in full (unquenched) QCD, the interquark energy in our holographic model also approaches a temperature dependent constant value at larger values of . This temperature dependent constant value decreases with temperature (from speciousconfined to deconfined), which again is in line with full QCD results (see for example Figure 1 of [12]). Although we do not have a clear understanding where this peculiar “mixture” of quenched vs. unquenched QCDlike behaviour is caused by precisely, it is not related to having a too small ’t Hooft coupling (or small ) that would cloud the dual gaugegravity interpretation: as we noticed before, the qualitative features of our models persist, independent on how one ultimately decides to choose by hand or fix on an external QCD variable the string tension, or similar quantity.
Another possibility might be that it is related to a wrongful identification of the scalar field with the dilaton, see discussion below eq. (2.16), but as discussed there, not making this identification would lead to a loss of all confiningrelated properties of our models.
3.3 Thermal entropy of a pair
We now move on to discuss the thermal entropy of a pair in the above speciousconfined/deconfined phases. This entropy can be calculated from the free energy via the relation,
(3.9) 
For black hole backgrounds, we have two choices for , corresponding to the two different behaviours of with respect to the separation length. For large separation, we have
(3.10) 
On the other hand for small separation, we have
(3.11) 
We will see that the two distinct behaviours of as a function of the separation length precisely capture the QCD results for the entropy in their respective regimes.
We now discuss a few silent features of the holographic calculations for the entropy and compare with the lattice QCD results:

The variation of with respect to temperature in the small black hole phase is shown in Figure 13. Here, we have fixed the separation length to . The essential features of our analysis remain unchanged for other values of , and is just a particular choice. We find that in this speciousconfined phase the entropy initially varies slowly at low temperatures, and then increases rapidly towards the critical temperature. It indicates a large amount of entropy associated with the pair near the critical temperature, as also observed in lattice QCD. We see that the holographic results for the entropy in this speciousconfined phase are qualitatively similar to those of lattice QCD. It also indicates the main difference compared to [47], where the entropy in the confined phase was reported to be zero. We again like to point out that the nonzero entropy in the speciousconfined phase here arises precisely due to the fact that the dual gravity background is a (small) black hole, which depends on temperature. In the usual AdS/CFT correspondence, the confined phase is generally dual to thermalAdS (without horizon and temperature) and therefore the entropy of quark pair is inherently zero in those confined phases.

The entropy of the pair as a function of temperature in the large black hole phase at large separation is shown in Figure 13. For this purpose we use eq. (3.10) for the entropy. We observe that similarly to the speciousconfined phase a large amount of entropy is associated with the pair near the critical temperature. Similar results in the deconfined phase were found in [47] using the improved holographic model of [26, 27] ^{9}^{9}9The temperature dependence of the entropy of a pair and of the string tension were also discussed in a dual phenomenological model in [85]. Unlike for our current model, the metric of [85] was chosen by hand and it displays no clear phase transition picture on the gravity side. Rather it relied on an effective potential approach.. We further find that the higher temperature asymptotics of the entropy in our model is similar to those of [47]. In particular, for , we find a tendency of a rise of with temperature as also observed in lattice QCD. Moreover, our analysis further predicts similar asymptotic behavior of in the presence of chemical potential too.

Another important lattice QCD result which the holographic model considered here correctly describes, is the increase in the entropy of the pair as a function of distance between them, see Figure 15. Here we have shown results in deconfined phase for three different temperatures. We see that for each case, increases with . Moreover, for large , saturates to a constant value and becomes independent of it ^{10}^{10}10In order to make it more readable, the magnitude of has been suppressed by a factor of 2 in region of Figure 15.. This is due to the fact that the disconnected string configuration has lower free energy at large separations, while it is independent of . Therefore, the corresponding entropy is also independent of . We see that these results qualitatively match with the results predicted by lattice QCD (shown in Figure 2). However, as opposed to the latter, the entropy here does not smoothly go to saturation. There is a discontinuity in the entropy at (denoted by dotted lines in Figure 15). This discontinuity in the entropy arises precisely due to the first order transition between the different string configurations at .

In Figure 15, the variation of the entropy as a function of the interquark distance for various values of chemical potential is shown. We do not have lattice results here to compare with. In this regard, these entropic results can be thought of as a original prediction from holography. We find that essential features of the entropy remain the same even with a chemical potential present. The entropy again saturates to a constant value at large separations. Also, increases with chemical potential. This suggest that the distance around which entropy saturates, increases with the chemical potential.
We end this section by summarising our main results obtained so far. Till now we showed that by considering the form of as in eq. (3.1), a small/large black hole phase transition in the gravity side appears which on the dual boundary side corresponds to a speciousconfined/deconfined phase. We showed that although there is always a shape connected string configuration in the speciousconfined phase, it is however the disconnected string configuration which is more favourable for large separation length. Interestingly, we find that in spite of the reported differences between the speciousconfined and standard confined phase, the entropy of the quark pair in the former phase is qualitatively similar to lattice QCD confined phase results. Similarly, in the large black hole phase when the temperature is sufficiently high, it is the disconnected string configuration which is more favourable at larger separation. The two disconnected strings describe the dissociation of a bound state into a quark and antiquark, thereby corresponding to the deconfined phase in the dual boundary theory. The small/large black hole phases therefore correspond to speciousconfinement/deconfinement phases, and the corresponding critical temperature is found to decrease with chemical potential. Moreover, the entropy of the pair in this phase is in qualitative agreement with lattice QCD results.
4 Case 2: standard confinement
It is instructive to also study the entropy by considering a different form of . In particular, in order to check the universal nature of the results presented for the entropy, especially for the deconfined phase, we will now study the entropy in a different holographic model where the gravity dual genuinely describes the confinement/deconfinement phases in the boundary theory. For this purpose we need to consider a different gravity solution. As mentioned earlier, the same can be achieved by considering different form of .
Let us now consider another simple form of , such as
(4.1) 
It is again straightforward to see that at the boundary , implying that the bulk spacetime asymptotes to AdS at the boundary. Near the boundary . Further, it can be explicitly checked that has the same asymptotic form for both and . The parameter in eq. (4.1) is fixed by demanding the critical temperature of the Hawking/Page (or the dual confinement/deconfinement) phase transition to be around at zero chemical potential.
Importantly, for , the equation for dilaton field in (2.14) can be solved explicitly
(4.2) 
Its near boundary expansion is
(4.3) 
and in terms of the dilaton potential can again be written as
(4.4) 
We repeat here once more that the phenomenological bottomup holographic models
we are considering are based on the (implicit) assumption that these phenomenological models are derivable from a consistent truncation of a higher
dimensional string theory. Therefore, the dilaton might be expected to be massless in a 5D truncated gravity theory (like ours) as well. Though, as frequently done, see e.g. [93, 94, 95, 96], the scalar dilaton can be associated to the dual scalar glueball state [97] described by , which is massive in QCD (or even pure YangMills gauge theory). In fact, whatever the dual of the dilaton would be, QCD(like) theories are not expected to have any massless physical degrees of freedom in their spectrum, at least away from the chiral limit. As such, it is no surprise that, to our knowledge, phenomenological holographic QCD models are frequently incorporating a massive dilaton as an easy access to a massive scalar glueball, let us refer to [96] for a recent discussion and relevant references. Another example with a massive dilaton is [98]. Seminal works using bottomup massive dilatons are [54, 53], there more in relation to QCD(like) thermodynamics than to glueball spectra. The mass was related to the (UV) anomalous dimension of . One of the considered dilaton potentials in [54, 53] was a simple exponential, as also discussed in [68], which evidently include a term upon expansion. A more refined version of the models considered here in our paper would be to ensure that the quadratic term in the expansion of is related to the anomalous dimension of instead of to the rather simple (and crude) value of reported now.
For completeness, also the of Case 1 gives rise a dilaton mass term in the potential that is consistent with the BF bound for a scalar degree of freedom, see eq. (3.2). In fact, up to order , the dilaton potentials of both Cases are identical.
4.1 Black hole thermodynamics
The thermodynamic results of the gravity solution with as in eq. (4.1) are shown in Figures 17 and 17. In this case no small to large black hole phase transition takes place. There are now only two branches in the plane. The branch with negative slope (small ) is stable whereas the branch with positive slope (large ) is unstable. The appearance of this unstable branch however depends on the value of the chemical potential and in particular it ceases to exist for higher chemical potential. This defines a critical chemical potential . Moreover, the black hole solution does not exist below a certain minimal temperature . This suggests a phase transition from black hole to thermalAdS as we decrease the Hawking temperature. The phase transition can be observed from the free energy behaviour, shown in Figure 17, where the same normalization as in the previous section is used. We see that the free energy is positive for the unstable branch and becomes negative after some critical temperature along the stable branch, implying a first order Hawking/Page phase transition from thermalAdS to AdS black hole as the temperature increases. The overall dependence of on is the same as in Figure 5, however with larger ^{11}^{11}11A similar kind of Hawking/Page phase transition with a planar horizon has been reported recently in [99]..
As we will show in the next subsection, this thermalAdS/black hole phase transition in the gravity side corresponds to the standard confinement/deconfinement phase transition on the dual boundary side. In particular, the thermalAdS phase corresponds to confinement whereas the black hole phase corresponds to deconfinement. Correspondingly, defines the dual transition temperature. By construction, our result at zero chemical potential agrees with its lattice estimate. Moreover, we find that the transition temperature decreases with the chemical potential which is again in qualitative agreement with the lattice results.
4.2 Free energy of the pair
We now discuss the free energy of the pair with as in eq. (4.1). Again, depending upon the background geometry, there can be both connected as well as disconnected string solutions. The equations for the connected (eqs. (3.5) and (3.6)) and disconnected string (eq. (3.7)) remain the same, except is replaced by eq. (4.1).
Let us first examine the free energy in the thermalAdS background. The results are shown in Figures 19 and 19. Again, just as for the small black hole background of the previous section, an “imaginary wall” appears and the connected string world sheet does not go deep into the bulk and tries to stay away from the singularity. Importantly, the free energy of the pair is again found to be of the Cornell type, . ^{12}^{12}12Again, one can fix the value of open string tension by comparing the lattice QCD result with our numerical results. By doing that we find . This suggests that the pair is connected by the string and forms a confined state in the dual boundary theory. However, as opposed to the small black hole background, here is actually always the true minimum of the NambuGoto action, which can be easily verified by noticing that the disconnected string solution has an additional IR divergence and therefore is never a relevant solution of NambuGoto action. In order to explicitly see this, let us first note the IR (large ) expansions of and ,
(4.5) 
(4.6) 
Substituting these expressions into expression, we have
(4.7) 
where