Generalised Planar Black Holes and the Holography of Hydrodynamic Shear
Generalised Planar Black Holes and the Holography of Hydrodynamic Shear
Brett McInnes and Edward Teo
National University of Singapore
email: firstname.lastname@example.org, email@example.com
AdS black holes with planar event horizon topology play a central role in AdS/CFT holography, and particularly in its applications. Generalisations of the known planar black holes can be found by considering the Plebański–Demiański metrics, a very general family of exactly specified solutions of the Einstein equations. These generalised planar black holes may be useful in applications. We give a concrete example of this in the context of the holographic description of the Quark-Gluon Plasma (QGP). We argue that our generalised planar black holes allow us to construct a model of the internal shearing motion generated when the QGP is produced in peripheral heavy-ion collisions. When embedded in string theory, the bulk physics is in fact unstable. We find however that this instability may develop too slowly to affect the evolution of the plasma, except possibly for high values of the quark chemical potential, such as will be studied in experimental scans of the quark matter phase diagram.
1. Holographic Description of the Internal Motion of the QGP
Collisions of heavy ions  are believed to produce a state of matter known as the Quark-Gluon Plasma or QGP. One theoretical approach to understanding this state is based on holography, in which the QGP is modelled by a field theory dual to a gravitational system, a thermal AdS black hole [2, 3, 4, 5]. Because the QGP exists in Minkowski space, one needs to use black holes with topologically planar event horizons; fortunately, these do exist in the asymptotically AdS case , though, as we shall see, these objects differ, in many important particulars, from their counterparts with topologically spherical sections.
The QGP, as produced in collisions, is far from being a static system: most obviously, it expands very rapidly, and much work is currently devoted to finding a dual description of the expanding QGP (see [5, 7, 8, 9, 10] and references therein). However, it has recently come to be appreciated that, in non-central (“peripheral”) collisions, the QGP is also subjected to an extremely intense shearing motion, because of the transverse non-uniformity of the colliding nuclei [11, 12, 13]. The large vorticity thus generated [14, 15, 16, 17, 18] may prove to have observable consequences, through quark polarization, and it may be important for forthcoming attempts to simulate peripheral collisions using holography .
Clearly it is important to determine what the holographic approach has to teach us about this shearing effect. Since the shearing imparts a very large angular momentum to the plasma, the natural suggestion  is to consider AdS-Kerr [21, 22] black holes in the bulk. However, while the AdS-Kerr black hole (with a topologically spherical event horizon) does induce rotation at infinity, the angular velocity is constant (that is, independent of direction) there, and hence there is no shear. This spacetime is indeed of interest for possible holographic descriptions of systems which are genuinely rotating (see  for an explicit example, and  for another potential application), but this is not what we seek here.
In any case, the AdS-Kerr metric does not have a conformal boundary which is globally conformal to Minkowski spacetime, so one should really begin rather with non-static black holes which do have that property — that is, with planar black holes possessing angular momentum. Such black holes were discovered by Klemm, Moretti and Vanzo , and one finds that, in addition to inducing a more reasonable geometry at infinity, these “KMV spacetimes” bring with them a major advantage: the angular velocity at infinity depends on one of the spatial coordinates, thus inducing an effective shearing motion on the boundary. The KMV spacetimes, and their electrically charged (“QKMV”) versions, are therefore prime candidates for building a holographic description of the shearing QGP. Such a description may be very important, because it often happens that certain effects are apparent on one side of a holographic duality, but obscure on the other. Work in this direction was described in [26, 27].
The shearing motion of a fluid is described by a velocity profile, an expression of the (dimensionless) velocity as a function of transverse distance from some axis. (In the case of plasma generated by heavy-ion collisions, it is customary to choose the axis to be that of the collision, that is, the axis along which the velocity vanishes; it is conventional to take it to be the -axis.) This function is of basic importance, since it describes the internal dynamics of the plasma. Unfortunately, in the extreme conditions in the aftermath of a heavy-ion collision, it is difficult to predict the precise shape actually takes; however, typical shapes arising in shear flows are known (see , page 133). Such a shape, chosen because it is consistent with causality, is shown in Figure 1.
Crucially, some aspects of fluid behaviour actually depend only on the general shape of the profile, not on the details; these aspects, therefore, can be discussed in the QGP case, even in the absence of a precisely specified function. Most important among these is the question as to whether the shearing motion described by is stable, in the hydrodynamic sense. Frequently it is not, the most well-known example being the Kelvin–Helmholtz instability, which is important in numerous fluid mechanics problems where shear causes a laminar flow to become turbulent. Remarkably, all one needs to detect this instability, in the case of a monotone profile, is a knowledge of the sign of the second derivative of . To be precise, a necessary (and usually sufficient) condition for Kelvin–Helmholtz instability to be present is that there should exist a value of such that the following is satisfied:
where is the location of a point where the second derivative vanishes. (This is the classical “Fjørtoft theorem”: see , page 132.)
Thus, for example, one should expect a fluid velocity profile like the one in Figure 1 to be unstable
We can summarise by saying that a detailed knowledge of the precise shape of is not required to make these statements about the locations in which shear-induced hydrodynamic instability should be expected to arise: it will suffice if we can understand the behaviour of fluids having velocity profiles with a given general shape (concave “up” or “down”). The physical intuition  here is simple (but very classical): if a fluid cell with large vorticity (such as those near a point of inflection in ) is moved slightly towards a region of lower vorticity, it will not tend to return to its original position.
It is clearly very important to understand whether shear-induced instabilities can affect the flow of the QGP arising from peripheral collisions. In a recently proposed theoretical model of the shearing QGP (see [30, 31] and references therein), it is suggested that the velocity profile does take a form satisfying the conditions of Fjørtoft’s theorem, and simulations of the consequent Kelvin–Helmholtz instability are generated. This may well lead to observable effects, and so one obtains, in principle, a way of testing the model.
This discussion is based, however, on assuming that the QGP is fully governed by classical hydrodynamics. In particular, it is assumed in [30, 31] that the instability is localised, as above, around points of inflection in the velocity profile. But it is not entirely clear that the QGP is governed by purely classical effects; in view of the many forms of instability well known to be associated with other plasmas, one should be prepared to encounter deviations from classical expectations in this case also. This is precisely the kind of question on which the holographic approach might be expected to throw some light, and, in fact, the theory of holographic corrections to classical hydrodynamics is currently a subject of great interest .
In this work, we will use the QKMV geometries, and generalizations of them, to construct the AdS/CFT duals of boundary configurations corresponding to classically stable velocity profiles of the kinds portrayed in Figures 2 and 3. The objective is to study whether the classical stability continues to hold when the bulk physics is considered.
The QKMV metrics actually induce velocity profiles at infinity of the form given by Figure 2, but never of the kind given in Figure 3. They are therefore unable to give a complete description of a realistic profile (since such a profile would certainly, by causality, correspond to a bounded function, so at least part of the full graph must be of the form given in Figure 3). However, Klemm et al.  obtained their metric as a special case of the Plebański–Demiański family of metrics [33, 34], the most general metrics of Petrov Type D , and therefore the most general spacetimes of black hole type that one is able to examine explicitly. The idea suggests itself that a metric inducing a profile like the one in Figure 3 may also be found as a more general member of that family. The suggestion that some of the less familiar Plebański–Demiański metrics may be physically relevant has indeed been explored recently [36, 37]. The results are encouraging, in that they indicate that these metrics have good properties from a supersymmetric point of view, and thus might ultimately be embedded in string theory.
In this work we exhibit a generalised planar black hole geometry of this kind. This geometry is characterised by its ADM mass, electric charge, angular momentum parameter, and by a new parameter conventionally denoted by . The physical meaning of this parameter is, in general, obscure
We find that a plasma with either of the profiles in Figures 2 and 3 is dual to an unstable system in the bulk: this is due to a specifically “stringy” bulk effect, the instability associated with the production of branes wrapping around transverse sections . The corresponding instability in the fluid is not localised near a point of inflection in the velocity profile. It corresponds to a rather dramatic transition to turbulence throughout the fluid.
However, one must always bear in mind that the QGP formed in any heavy-ion collision is inevitably a very short-lived state. We propose a holographic method of estimating the time required for our non-classical instability to develop, and find that, under the conditions of experiments performed hitherto, this time may well be too long to affect the plasma before it hadronises. If that is so, the idea that hydrodynamic instability arising from shear is localised in the manner proposed in  is valid for these experiments. The instability revealed by holography does however develop much more rapidly when the quark chemical potential is large; this is interesting, because plasmas with large chemical potentials are the subject of much experimental interest, in the “beam energy scan” programmes projected for such facilities as RHIC, SHINE, FAIR, and NICA [39, 40, 41, 42, 43]. It is possible that, under these conditions, the plasma will behave in a manner quite different from predictions based on a simple Kelvin–Helmholtz effect.
2. The Boundary Geometry
A simple argument, presented very clearly in , shows that, as a result of the non-uniformity of the distribution of nucleons in the transverse direction, the QGP produced in a peripheral heavy-ion collision acquires a very large angular momentum density associated with a non-trivial transverse velocity profile. Planar black holes with non-zero angular momentum, first described in , do not actually “rotate”: they are characterised by a shearing motion in each transverse section strictly outside the event horizon. These planar black holes
More generally, a planar black hole will be of interest for this purpose if it induces at infinity a “peripheral collision geometry” with a metric of the form
Here and are Cartesian coordinates describing a typical section through the plasma, with being the axis of the collision which produced that plasma; the function is the asymptotic value of the angular velocity of the black hole (so we want this function to vanish along the axis, that is, for = 0). It depends on , so that the velocity profile is not trivial; it also depends on various parameters of the underlying black hole, such as its angular momentum, and on , the asymptotic AdS curvature scale.
Free particles in the spacetime described by the metric in (2), with = constant and zero momentum in the direction, nevertheless move in the -direction at a dimensionless speed given by
so the function describes the velocity profile at infinity. This motion is just the usual frame-dragging associated with any black hole with angular momentum: but the essential difference between asymptotically flat and asymptotically AdS black holes is that, in the latter case, frame-dragging persists even at infinity. This frame-dragging at infinity opens up the possibility of using the AdS/CFT duality to study rotating matter in the topologically spherical case , and shearing matter in the topologically planar case.
Let us see how this works in the special case of the asymptotically AdS black hole geometry given by Klemm et al.  (actually, we will use the electrically charged version, which we call the “QKMV” metric). That metric takes the form
where the asymptotic AdS curvature is , where and are dimensionless planar coordinates, and where
Here and are the mass and charge parameters, defined in terms of densities at the horizon (so that, for example, the charge density at the horizon is given by , where , the value of at the horizon, is the largest root of ; see  for this procedure, which is necessitated by the non-compact topology of the sections here.) Similarly, the parameter is the ratio of the angular momentum and energy densities at the horizon.
Taking the limit, and defining Cartesian coordinates by d = d and d = d, one finds  that the conformal boundary metric is given precisely by equation (2) above, with asymptotic angular velocity function defining a velocity profile given by
with = , and where sinl( sn( is the “lemniscatic sine”, one of the Jacobi elliptic functions , sn(), with imaginary elliptic modulus. (This function is real, periodic, but not bounded here, since it is being evaluated off the real axis.)
Choosing typical parameter values, one obtains the QKMV velocity profile, pictured in Figure 2. All of the velocity profiles obtained from QKMV metrics are of this shape. Notice that there is no point of inflection here, even at the origin; this can easily be shown directly from the properties of the Jacobi elliptic function (or by using equation (9), below). Thus a fluid with this profile is classically stable.
We are therefore in a position to give a holographic account of fluids with profiles like those in Figure 2. Our task is now to find some new bulk geometry such that, in a similar manner, a profile of the form shown in Figure 3 can be obtained. We shall do that in the next section, but first we study the (surprisingly strong) constraints imposed by the physics of the boundary field theory.
We begin by noting that the QKMV boundary metric is not flat, but (as we will see) it is conformally flat, like the boundary of the topologically spherical AdS-Kerr-Newman spacetime, which is used to study rotating superconductors . Unlike the latter, it actually is globally conformally flat
As we try to generalise the QKMV metric, then, we should do so in a way that preserves the conformal flatness of the boundary. Let us investigate the conditions under which a general metric of the form given in equation (2) can be conformally flat. The condition for this  is the vanishing of the Cotton tensor,
where is the alternating tensor and is the Ricci tensor. It is clear that requiring this object to vanish for the metric in equation (2) will impose a third-order differential equation on ; the equation has the form
where the dash denotes a derivative with respect to . Since does not appear explicitly, one constant of integration will be trivial (constant translations of ); the other two will be the physically significant ones.
Surprisingly, this complicated equation can be reduced to a first-order equation: see  for the details. One finds that all solutions of equation (8) are either constant or solutions of the equation
where and are dimensionless constants. Because should vanish at , we see that , so is either zero or positive; similarly must be positive if ; otherwise and are arbitrary: they are the two constants mentioned above.
The function sinl) satisfies equation (9) with , and so, if we set (which means that the parameter has to be positive in this case), we get exactly the expression in equation (6). This confirms that the QKMV boundary is conformally flat (and it gives us the physical interpretation of the constant , in terms of the angular momentum parameter of the underlying planar black hole).
On the other hand, setting = 0, we obtain an equation which can be solved in terms of an elementary function:
The graph of this function is similar to the one portrayed in Figure 2, so this geometry, too, describes the part of the graph in Figure 1 with small . This case does have one unique feature: the graph, like that of a realistic profile, does have a point of inflection at . However, the condition in Fjørtoft’s theorem is not satisfied even here, so, once again, a fluid with this profile is classically stable. It is easy to see that similar results are obtained if both and are positive: all of the graphs will resemble Figure 2. All of these geometries (, ; , ; and ) are candidates to describe that kind of profile.
One possibility remains: that should be positive, and negative. Clearly the slope of the graph in this case gradually decreases, until a maximum is reached. If we cut off the solution at that point, then we can expect to obtain a graph like the one in Figure 3. This case therefore plays an essential role: apart from any other consideration, the velocity is bounded in this case (only), so causality is respected. This is the case on which we focus for the remainder of this section.
It will be convenient to adopt a new notation at this point. Let us use the velocity directly, instead of the asymptotic angular velocity, as in equation (3). Next, replace by , as above in our discussion of the QKMV case, except that now the parameter must be negative. Finally, for reasons which will become clear, we wish to replace by 2, where is a new parameter, with units of length, which remains to be interpreted
where is a constant defined by
It is clear from equation (11) that has a simple physical interpretation: it is the maximal velocity of the plasma, some large fraction of the speed of light in the case of a heavy-ion collision. Inspection of (11) also reveals that the parameter determines how rapidly the velocity changes with respect to the coordinate , so it is a numerical measure of the quantity of shearing to which the plasma is subjected; this is consistent with its dual interpretation (see above) as the angular momentum parameter of the dual black hole, assuming that there is one. The combination is related to the value of the coordinate when reaches its maximum, so it is a measure of the transverse dimension of the interaction zone. Thus, all of the factors on the right side of equation (12) are understood, and so we now have a physical interpretation for : it is a length scale determined by the transverse size, maximal velocity, and angular momentum of the shearing plasma.
Equation (11) can be solved exactly, in terms of the Weierstrass -function . This function is characterised by a pair of numbers, and , called the elliptic invariants, so that the function is expressed in general in the form . The solution is then
Here is a constant chosen so that the graph passes through the origin.
Now bear in mind that the QGP exists only in the narrow strip , where is defined as half of the extent of the overlap of the two colliding nuclei; clearly can be computed from the transverse size of the nucleus and the impact parameter. Then attains its maximum at the edge of this strip: that is, , or
Combining this equation with , we have a pair of simultaneous algebraic equations, from which the remaining parameters in equation (13) can be computed, given , , and ; and so the shape of the velocity profile (in Figure 3, or the upper part of Figure 1) is fixed
Note that the solution curve in this case has no point of inflection. One can see this from equation (11) itself: differentiating and simplifying, we have
which does not vanish. Therefore, once again, we are dealing with a classically stable fluid motion.
We see, then, that if we wish to use frame dragging at infinity to model the internal shearing motion of the QGP, then the boundary geometry is very tightly constrained even in the absence of detailed knowledge of the bulk geometry. In fact, since the function is essentially the one non-trivial component of the boundary metric tensor in these coordinates, the boundary geometry is now completely determined, given physical data about the plasma and the region in which it forms. (Here we are leaving aside the problem of fitting Figures 2 and 3 together to obtain Figure 1; the complications arising from this will not affect our discussion, since our conclusions can be derived from considering each piece separately.)
In summary, the classification of possible “holographic velocity profiles” is complete: it is given above in terms of the classification of possible solutions of equation (9). We have a holographic dual for profiles like those in Figure 2, and we can hope (see below) to find a dual for profiles of the type given in Figure 3. The holographic approach is therefore complementary to the classical methods used in [30, 31], in the sense that it describes the situation everywhere in the fluid except near to the zone where the Kelvin–Helmholtz instability is expected to arise.
It was argued in  that, when string-theoretic effects are taken into account, the KMV black holes are unstable, and we will see below that the same is true of the QKMV geometries, for all values of the charge. We need now to ask whether this instability afflicts black holes inducing at infinity profiles like the one in Figure 3; of course, that entails demonstrating that such black holes actually exist.
3. The Generalised Planar Black Hole Geometry
The QKMV geometry discussed above was obtained  as a special case of the Plebański–Demiański family of metrics . The latter has been expressed in a more convenient form by Griffiths and Podolský [34, 35]. It is this form that will be used here: see Appendix A for a brief review. Our objective is to find a member of this family which is asymptotically AdS and which induces a boundary geometry of the form (2), with such that equation (11) is satisfied.
Now we require the term to vanish at . This is achieved by performing the shift , resulting in the metric
and , are given in (80) with . and should be positive to have the correct metric signature.
To obtain a planar metric, we require to be a constant. This implies two conditions on the parameters and :
This last condition is especially interesting, because it actually expresses the condition that the boundary will be conformally flat. In other words, if a bulk metric of the form (76)–(80) induces a boundary metric of the form given in equation (2), then that metric will automatically be conformally flat.
The remaining free parameter can then be chosen to set . Together with the values (20), we have
In particular, note that is manifestly positive. The bulk metric (76) then becomes (replacing and )
Here and have slightly different physical interpretations from their QKMV counterparts: for example, the charge density is rather than , where as usual locates the event horizon.
If we perform the shift , (22) can be written in the form
The corresponding electromagnetic potential is
It is easily checked that (26) formally
The positivity of can be checked by first rewriting it in the form
where the ellipsis denotes terms independent of . We immediately see that this is an increasing function of for positive . Moreover, the expression of in (27) shows that it is positive on the horizon (defined by the largest root of ), so it is positive everywhere outside the event horizon. It is clear that this geometry represents a well-defined planar black hole.
Note that the angular velocity of the event horizon is , where at the event horizon. It is independent of position there, but not at any other value of , including infinity.
The special case , merits attention, because of its great simplicity. Notice first that the metric is still non-diagonal in this case, so is more like angular momentum than electric charge in this case (see  for the corresponding statement in the spherical case). If we set , then . The boundary metric (18) then becomes
This is precisely the boundary geometry we discovered in the preceding section in the special case , , which means that this particular boundary geometry does have a dual interpretation in terms of a black hole in the bulk.
In fact, this statement holds true even when . To see this, we need to express the QKNV boundary metric explicitly in the form given in equation (2). Notice first that in this case we have
Next, define a new coordinate by
Setting , differentiating , and squaring, we get
A lengthy algebraic manipulation allows us to combine these equations to obtain
Defining, as usual, by , and as in equation (12), we see that we have again obtained equation (11) in the preceding section. There we obtained it from general properties of the boundary physics; here it arises from the bulk geometry. The Griffiths–Podolský parameter has turned out to be precisely the constant we obtained by solving the equation expressing the conformal flatness of the boundary. In other words, the geometry we discussed in the preceding section does have a bulk dual: that dual is just the QKMV geometry. To put it yet another way: the boundary metric of the form given in equation (2), with given (after dividing by ) in equation (13), can be obtained by replacing the QKMV geometry by an QKMV geometry, also in the Plebański–Demiański class. The result is to replace Figure 2 by Figure 3 for the velocity profile at infinity.
As a side-benefit, acquires a clear physical interpretation in terms of the physics of the boundary field theory: as we saw earlier, it is a length scale computed in terms of the maximal dimensionless velocity of the plasma, its angular momentum per unit energy, and the AdS curvature scale. Notice however that causality in the boundary field theory, expressed as , imposes a bound on the ratio , namely
This looks rather restrictive from the bulk point of view, since the QKMV metrics violating it are classically well-defined. Later (Appendix B) we shall see, however, that there is good reason to impose this condition even in the bulk.
We see, then, that the QKMV geometries give rise to all of the conformally flat boundary geometries with velocity profiles as in Figure 3. This is at first sight surprising, because the Plebański–Demiański geometries we have considered are by no means the most general ones: we have assumed, merely for simplicity, that the “acceleration” parameter (see Appendix A) vanishes. Since we have just seen that the bulk geometries already account for all possible boundary geometries of the kind we need, it follows that taking cannot lead to anything new; the QKMV geometries are the most general ones of Plebański–Demiański type inducing boundary geometries representing the QGP generated by a peripheral heavy-ion collision.
In order to complete the holographic dictionary in this case, we need to show how the bulk parameters and can be computed from boundary data. Here the temperature and chemical potential of the boundary field theory are relevant. To compute them, it is as usual convenient to transform to the Euclidean domain, which we now explore.
4. Temperature and Chemical Potential
We now discuss the Euclidean version of the QKMV geometry. We will need this to compute the temperature of the black hole, but it is also needed for studying the chemical potential of the boundary field theory, and to compute the action for certain branes propagating in the bulk. Technically, our focus is on the periodicities of the Euclidean versions of the non-radial coordinates (including time).
To understand the Euclidean version of the coordinate , it is best to consider the situation on the boundary. The Euclidean version of equation (11) is
note that and , being time derivatives, have to be complexified (in the same way as and , that is, , , , ). This remarkable differential equation has two disjoint sets of solutions. One set consists of unbounded functions, bounded below by unity; these are the functions one obtains by complexifying the parameters in the Weierstrass -function in equation (13). These are of no interest here, since they will not define a complete Euclidean metric. The other set consists of functions satisfying . The solution in this case takes the form
where is arbitrary and sn is, as mentioned above, one of the Jacobi elliptic functions ; here
This solution was obtained by performing a fractional linear transformation in to turn (37) into a well-known differential equation whose solution is just sn.
Now sn is periodic on the real axis, hence the same is true of : in other words, the coordinate is compactified in the Euclidean case. Its period can be computed from the period of sn, usually stated in terms of the complete elliptic integrals of the first kind . However, the periodicity can be stated more usefully in terms of the period of the Euclidean version of the coordinate . (Note from the Euclidean version of equation (33) that can be expressed in terms of , to which is proportional.) Using the Euclidean version of equation (32), one sees that, as passes from one minimum () to the next, varies between and , where
4.2 Euclidean and
The Euclidean versions of the coordinates and are best studied in the bulk.
The Euclidean version of the bulk metric (26) is
We may call this the “QKMV gravitational instanton”. The corresponding Euclidean electromagnetic potential is
If denotes the value of the radial coordinate at the Euclidean event horizon, then
and can be written in the alternative, factorised form:
To ensure a positive definite signature, we restrict ourselves to the range and , where are roots of , appropriately chosen from the four possibilities . (Note that the quantities we previously called and correspond to a particular pair chosen from these four.) In particular, these ranges will ensure that and the second factor of (50) are positive.
Recall that we need . There are two separate cases to consider: and . The first case is the physical one here: the second would violate causality on the boundary, as we discussed earlier (inequality (36)). It turns out (see Appendix B) that the second case is also unacceptable from the bulk point of view, because it does not correspond to a well-defined gravitational instanton. We therefore confine ourselves here to the first case. In this case, the relevant (real) roots of are precisely those given in equations (40) above.
Now since the QKMV gravitational instanton has two commuting Killing vector fields and , with their associated fixed points at and , it has a isometry group. A well-developed formalism (see ) of “rod structures” has been constructed to deal with such gravitational instantons, and we will use it here. Briefly, this formalism assigns a sequence of so-called rods to a given gravitational instanton, with each rod having a certain direction . Each rod actually represents a two-dimensional fixed point set of the isometry subgroup generated by its direction. It follows that points at which two adjacent rods meet are fixed points of the whole isometry group.
It can be checked that the rod structure of the QKMV gravitational instanton consists of the following three rods:
Rod 1: a semi-infinite rod located at , with direction
Rod 2: a finite rod located at , with direction
Rod 3: a semi-infinite rod located at , with the same direction as Rod 1: .
The pair , or equivalently the pair , generates the isometry of this gravitational instanton.
Let us quickly work out the explicit identifications imposed on the coordinates by this isometry, and the requirement that the gravitational instanton is regular. If we change coordinates
the two linearly independent rod directions take the “orthogonal” form:
In order to avoid conical singularities along the rods, we then have to impose the following two independent identifications:
In terms of the original coordinates , these two identifications are
both of which non-trivially mix the two coordinates.
It can be seen from the above rod structure that constant and sections of the gravitational instanton are topological two-spheres parameterised by , with the two “poles” at . It follows that the constant sections have topology. In particular, the boundary of the QKMV gravitational instanton inherits this compact topology.
4.3 Temperature of the Qkmv Planar Black Hole
As usual, the temperature of the black hole Hawking radiation (see ) can now be computed from the periodicity of Euclidean “time”: we find, after continuing back to the Lorentzian section,
Recall that can be expressed in terms of the parameters , , and , all of which can be computed from field theory data on the boundary, and that is related to the other parameters by the equation ; in the zero-charge case we can now compute given the temperature. In the charged case, however, we need another equation, relating the charge parameter to physical data. We now turn to this.
4.4 Relating the Charge Parameter to the Field Theory Chemical Potential
The Euclidean electromagnetic potential form in the QKMV geometry was given earlier (equation (48)). It can be expressed more generally as
where and are constants corresponding to a choice of gauge; notice that they also give the asymptotic value of . Now recall from the rod structure formalism that the norms of both and vanish at those points where the rods intersect; that is, when and (or ; see equations (40)). Since the geometry is indeed Euclidean, this means that the vector fields and themselves vanish at these points, which in turn means that there; hence we see that, if is the value of at and , then
After some simplifications followed by complexification one can obtain the Lorentzian versions of these quantities, and so evaluate the asymptotic electromagnetic potential form:
This can be used to compute the electric potential with respect to any given choice of observer at infinity. We are particularly interested in the observer who is at rest relative to the axis of the collision, whose worldline has unit (with respect to the boundary metric) tangent vector ; in the AdS/CFT dictionary, the quark chemical potential is proportional  to the asymptotic electric potential seen by this observer. Evaluating on , and regularizing the units according to , we obtain finally
Given the temperature, chemical potential, and angular momentum per unit energy of the boundary theory, we now have three equations (equation (60), , and equation (65)) for the three unknowns , , and . In short, the bulk geometry is now fully computable from the boundary data.
5. Branes in the Qkmv Geometry
According to the AdS/CFT duality, string theory on the background defined by the black hole we have been discussing is equivalent to the physics of a certain field theory on a specific conformally Minkowskian geometry, of a kind which can be used to model a system undergoing shear. That field theory is not QCD, but one can hope, with due caution [52, 53, 54], that the differences are not so great as to render the comparison valueless. In short, the behaviour of string theory on the QKMV background might have something new to teach us about the shearing QGP.
One of the most characteristic properties of (Euclidean) asymptotically AdS spaces is that the areas of surfaces are comparable to the volumes they enclose, as they expand towards infinity. This becomes a directly physical effect in string theory, because of the presence of branes wrapping around such surfaces.
The action of a brane has a positive contribution from its tension (related to the area) but also a negative contribution from the enclosed volume (due to the coupling to the background). This negative term does not lead to any pathologies in AdS itself, but Seiberg and Witten  pointed out that it might do so, for BPS branes, in spaces which are only asymptotically AdS: the geometric deformation might upset the delicate competition between the area and volume terms, allowing the latter to dominate, leading perhaps to a brane action which is unbounded below. If that should happen, the resulting pair-production instability would correspond, through the AdS/CFT correspondence, to the existence of some kind of instability in the field theory. Because of its generality, this is a very important effect, and it has been used to address some fundamental issues in AdS/CFT theory (for example, see ).
This issue was considered in the case of the KMV geometry in . We found there that this effect does arise in that case. The question is whether this is also true of the QKMV and QKMV geometries, and, if so, for which values of the new parameters.
In the case of the Euclidean version of the QKMV geometry, we can compute the Seiberg–Witten action for a brane wrapping a compact transverse section at any fixed value of the radial coordinate : it takes the form
Here is a constant whose precise value need not detain us
Evaluating the integrals, we have
After an analytic continuation back to Lorentzian signature, the physical brane action is found to be
By construction, this action vanishes at the event horizon, and it is positive at first as increases. But it does not remain positive: eventually the graph of the action as a function of turns over and cuts the horizontal axis. In fact, at large , behaves as
where is a certain positive constant. Since is less than unity, we see that the graph at large is essentially that of a straight line with negative slope, so it will ultimately cut the horizontal axis and remain negative. In short, the brane action is unbounded below at large values of , and the system is unstable to brane pair-production  for all non-zero amounts of shear, in all of the QKMV and QKMV geometries
The final conclusion is that, according to holography, both of the flows portrayed in Figures 2 and 3 are unstable. It follows that a realistic flow for the QGP in the aftermath of a heavy-ion collision, such as the one shown in Figure 1, is unstable not just in the centre, where there is certainly a Kelvin–Helmholtz instability, but throughout the flow field. In short, holography suggests that classical hydrodynamics may be misleading us here, in a somewhat dramatic manner.
However, such plasmas exist, in any case, only for a very short period of time (of the order of 5 fm/c, though somewhat longer in the most energetic LHC collisions). The simulations in  indicate that classical instabilities in the QGP flow develop extremely rapidly, and it is clear that they must do so if the effect is to be physically relevant. If the instability we have been discussing does not likewise evolve very rapidly, then it will not influence the results of any experiment. Thus, we cannot draw any conclusions until we have some way of estimating, even very roughly, the time scale for the development of Seiberg–Witten instability. We suggest that holography itself provides such an estimate, as we now explain.
6. A Holographic Estimate of the Time Scale
Using the holographic duality to estimate time scales in the evolution of strongly coupled systems is a well-established procedure; see for example  and references therein. In this spirit, let us try to estimate time scales for the hydrodynamic instability we discussed in the preceding section, by studying the evolution of the bulk instability we identified there.
We saw that the problem arises at large values of : that is to say, not in the immediate vicinity of the black hole. One can picture the situation as follows: the black hole is surrounded by a “screen”, with a location determined by the value of the radial coordinate where the brane action cuts the horizontal axis: the system only misbehaves, initially, outside this screen.
Now in AdS/CFT duality, the boundary theory is dual to (at least) the entire bulk system outside the event horizon. The suggestion is that the time required for the boundary instability to dominate should correspond to the time required for the region outside the black hole but inside the screen to be overwhelmed by the dynamics of the region of negative action. This in turn can be crudely estimated by asking how long it takes for a particle to fall through the screen to the event horizon. The region of negative action is defined by , where is the value of at which the action function vanishes: this is the location of the “screen”. Thus we are asking for the proper time required for a particle to fall from to , the location of the event horizon.
There is a technical complication here, arising from the fact that, like any black hole with non-zero angular momentum, the QKMV black holes are not isotropic: that is, just as the ordinary Kerr metric is not symmetrical in the latitudinal direction, the QKMV black hole is not symmetrical in the direction. What this means is that, in general, a geodesic beginning at a point with a given value of the coordinate will not maintain that value as the geodesic is extended towards the event horizon. At the boundary, this means (see equation (32)) that the corresponding observer’s velocity changes with time; that is, we would be computing times relative to a non-inertial observer. To solve this problem, we must begin with a value of which does not change, so that we are dealing with an inertial boundary observer. The times thus found can be converted to the laboratory frame by means of a Lorentz transformation.
If we define , then one can readily verify that the QKMV geometry is symmetrical in , in the sense of being invariant under ; in other words, the geometry is symmetrical about . It follows that the hypersurface is totally geodesic — a geodesic initially tangential to that surface will remain in it
With all this in mind, let us proceed. We take it that the object has zero momentum initially. It is initially at rest in the radial direction, and permanently, as above; due to frame dragging, however, zero momentum in the direction does not imply that is a constant. The existence of the two Killing vector fields, and , gives us two constants of the motion ( in the first case, zero in the second, by assumption):
Here the dot denotes a derivative with respect to proper time. The fact that the tangent of the geodesic, parametrised by proper time, is a unit vector, gives us a third equation. These can be combined to obtain , , and . The solution for gives us, after some simplifications and with the addition of the Lorentz factor, the time we seek:
Here has its usual meaning, and is to be fixed by the requirement that should vanish at . The expression depends on the parameters and , but we now know how to fix these, as well as , in terms of boundary data. Finally, can likewise be computed from those data, by setting the expression in equation (70) equal to zero. Thus can be determined, given physical information regarding the boundary theory.
Let us try to implement this idea with actual estimates of the relevant numbers. Even if, as seems very probable, the results are too rough to provide anything more than a qualitative impression of the time scale itself, they might yield hints as to whether it roughly of a magnitude such that the instability can affect the plasma before it hadronises; furthermore, it seems likely that they could give a useful indication of trends in the time scale as the parameters of the black hole are modified — that is, by duality, as the physical parameters of the boundary theory are varied. Such variations are in fact the subject of current and near-future experimental programmes (“beam energy scans” of the quark matter phase diagram).
In , we used data from the RHIC experiment  to estimate a maximal possible value of the angular momentum density in the relevant collisions of 360/fm; maximal in the sense that the impact parameter was chosen so that the angular momentum transfer to the plasma should be as large as possible (see ). Since a generic collision will give rise to somewhat lower angular momenta, and because the beam energy scan experiments involve less energetic collisions, we use 15 fm (based on an energy density estimate of 3 GeV/fm) as a conservative estimate for in a typical collision. Assuming that the impact parameters of the most relevant collisions here have values centred on the optimal value given in , one can compute the diameter of the corresponding interaction zone for gold nuclei; half of this is the range of the coordinate in Figures 1-3, and a reasonable estimate is about 6 fm. The full ranges of the temperatures and chemical potential values to be explored in the beam energy scan experiments are not known precisely, but it is safe to assume that they will be contained in the region , , both in units of fm.
Finally, we need to estimate , the maximal velocity of the plasma. This is more difficult, because there may be considerable deceleration during the brief interval after the collision but before the hydrodynamic regime begins. Following , we take 0.4; the associated value of is 11.35 fm. The results are mildly sensitive
With these parameter choices, which have been made mainly for illustrative purposes, we have computed the relevant values of for both the QKMV and the QKMV geometries (that is, for flows of the forms given by Figures 2 and 3 respectively). We find that the results do not differ very greatly in the two cases; they are shorter in the QKMV case, by roughly 10%
The results are shown in the table: times are in units of fm (usually denoted by fm/c).
|= 0||= 1||= 2||= 3||= 4||= 5|
Recall that the QGP is expected to survive for a time of the order of 5 fm/c, though somewhat more in very energetic collisions. Again, we stress that the numerical values should be trusted only on the qualitative level: the trends, however, are more reliable. The most striking trend is of course the remarkable decrease in as increases and decreases, as will happen in the beam energy scans [39, 40, 41, 42, 43]. Intuitively, the screen around the black hole in the bulk is “thinned” by larger values of its electric charge, particularly at low Hawking temperatures; the dual of this phenomenon produces the pattern in the table.
A reasonably conservative interpretation of these results is the following. The model suggests that, contrary to expectations based on classical hydrodynamics, the flow of the QGP is unstable throughout the fluid. However, it may be that this non-classical instability arises too slowly to be important when the quark chemical potential is very small — as it has been in most observed collisions to date. The situation is less clear, however, for the larger values of being investigated in current beam energy scan programmes, or in those of the near future, since the time required drops rather dramatically under those conditions. Our tentative conclusion is that, as assumed in , the plasma flow is effectively stable, away from the point of inflection in the velocity profile, at low values of ; but that it is not safe to assume this in future experiments involving very high values of .
In this work we have exhibited planar black holes of the Plebański–Demiański form, and we have shown how they may be physically interpreted in the context of the holographic description of strongly coupled fluids. We have found that these bulk spacetimes induce boundary geometries which correspond to shearing motions of such a fluid. These motions have velocity profiles corresponding to regions of the flow field where the classical Kelvin–Helmholtz instability cannot arise; and yet the bulk physics is unstable when a characteristically string-theoretic effect, involving branes, is taken into account. However, it is not clear that the plasma endures for a sufficiently long time for this latter effect to become important observationally.
Fluid instability normally represents a transition from laminar to turbulent flow. Let us suppose that the QGP does make such a transition at high , before it hadronises, in a manner describable dually by the Seiberg–Witten effect. Then, as we have seen, this should occur throughout the fluid, and not merely deep in the fluid field. This might well have important consequences: for example, it could affect the “spectator