Snapping Swallowtails in Accelerating Black Hole Thermodynamics
The thermodynamic behaviour of a charged and accelerating AdS black hole is studied in the context of extended phase space with variable cosmological constant. When compared to the charged AdS black hole without acceleration, a remarkable new feature of ‘snapping swallowtails’ appears. Namely, for any black hole with charge and any string tension causing the acceleration of the black hole, there exists a transition pressure at which the standard swallowtail ‘snaps’, causing the branch of low temperature black holes to completely disappear, leading to a pressure induced zeroth order phase transition between small and large black holes. For intermediate values of the string tension, we also observe a reentrant phase transition, as the small black hole changes to a large one and then back to small, as the pressure decreases, crossing the coexistence line of the two phases several times. We also find a new class of ‘mini-entropic’ black holes, whose isoperimetric ratio becomes unbounded in a certain region of parameter space.
The discovery that black holes can be assigned thermodynamic temperature  and entropy [2, 3] inaugurated the era of black hole thermodynamics. Featuring radiation that is universal over all particle species, an entropy that is proportional to the black hole area rather than volume, and negative specific heat, black hole thermodynamics has continued to be full of surprises. Especially interesting are the thermodynamic properties of black holes in asymptotically AdS spacetimes. These objects are known to exhibit interesting phase behaviour [4, 5, 6], relevant for the description of strongly coupled CFTs via the AdS/CFT correspondence .
Moreover, in AdS black hole spacetimes one can consider the negative cosmological constant to be a thermodynamic quantity whose variation gives rise to an additional pressure–volume term in the first law of black hole thermodynamics [8, 9, 10, 11, 12, 13, 14]. This is done via the identification
relating to the thermodynamic pressure . The subsequent study of black hole thermodynamics in this extended phase space has revealed remarkable similarities between the phase behaviour of black holes and that of ordinary matter .
where stands for the thermodynamic volume of the black hole, a quantity conjugate to the thermodynamic pressure , and and are respectively the black hole mass, temperature, entropy, electric potential, and charge. In a canonical (fixed charge) ensemble the system displays a small black hole to large black hole phase transition, fully analogous to the liquid/gas phase transition of the Van der Waals fluid . Namely, for pressures below a critical pressure, , the free energy of the system exhibits swallowtail behaviour, characteristic of the first order phase transition. The two black hole phases that meet at the ‘bottom of the swallowtail’ discontinuously differ in horizon radius. The corresponding phase diagram (the diagram) reproduced in Fig. 1 exhibits a coexistence line, which emanates from the origin and terminates at a (standard) critical point, characterized by the critical temperature and pressure
At this critical point the phase transition becomes of the second order and is characterized by the Ising universality class mean field theory critical exponents .
Remarkably, the Van der Waals-like behaviour has since been observed for many rotating and/or charged AdS black holes in various spacetime dimensions and for various gravity theories, and although more complicated phase behaviour may occur (see  for a review), it can be considered as a “prototype of thermodynamic behaviour” of AdS black holes in a canonical ensemble. For this reason it is rather instructive to find a departure from this prototypical behaviour and seek more complicated phase diagrams for AdS black holes, reflecting thus a more complicated behaviour of the dual CFT. To this end the following features have been identified: reentrant phase transitions , triple points analogous to that of water , an isolated critical point , and superfluid-like behaviour .
In this paper we investigate the thermodynamic behaviour of charged accelerating AdS black holes. The history of accelerating black holes goes all the way back to the early days of general relativity to the discovery of the C-metric [20, 21]. This metric has played an important role for many developments in general relativity, has been rediscovered many times (see  for references), and is understood now to describe accelerating black holes. The C-metric yields an example of an exact radiative spacetime and was exploited to study radiative patters in spacetimes with various asymptotics e.g. . It has been used to study black hole nucleation in various backgrounds [24, 25], to provide the means for splitting a cosmic string [26, 27], and in a generalized form was used to construct 5-dimensional black rings .
We shall restrict our attention to charged slowly accelerating AdS black holes. The associated C-metric is a special case of the general Plebanski–Demianski class of solutions of the Einstein—Maxwell equations . It describes a single accelerated black hole in AdS space that is suspended on a “cosmic string” represented by a conical deficit on one of the polar axes. Since there is only one horizon (no acceleration or cosmological horizons are present in the limit of slow acceleration), the system has a unique temperature and thermodynamics can be defined [30, 31] (see also [32, 33, 34, 35, 36, 37] for prior investigations). The key observation is that the tension of the string, that causes the black hole to accelerate, can be treated as (yet another) thermodynamic quantity whose variations add a new term to the first law 2, which now reads
where is a conjugate thermodynamic quantity to , known as the thermodynamic length .
As we shall see, the presence of acceleration has far-reaching consequences for the phase behaviour of charged AdS black holes. Let us first consider tiny acceleration (small string tension). In this case we find that the high pressure phase behaviour remains qualitatively similar to that of the non-accelerating charged black hole (with swallowtails and a critical point at above). However, a fascinating novel feature occurs at low pressures: for any charge and tension , there exists a critical pressure
at which the swallowtail ‘snaps’. As the pressure decreases below , the entire branch of small stable low temperature black holes disappears, breaking the structure of the swallowtail, and a new branch of unstable high temperature black holes emerges. This corresponds to a breaking of the co-existence line in the plane, which now no longer continues all the way to the origin but rather terminates at a new “critical point”, at , c.f. Fig. 1 with Figs. 7. Since the lower branch of the swallowtail is absent, a “no black hole” region at low temperatures emerges for . Moreover, there is a small range of temperatures, between and , where the global minimum of the free energy “jumps” as it crosses , corresponding to a zeroth order phase transition from small to intermediate black holes. Since the lines of coexistence of the first and zeroth order phase transitions merge at the point (as we shall illustrate below) we shall refer to this point as a “bicritical point”.
For small tensions we have . As the tension of the string increases, the bicritical and the (standard) critical point move closer to each other, with the former moving towards higher temperatures and pressures and the latter towards lower temperatures and pressures. At the same time the coexistence line of the first order phase transition exhibits a change in convexity and starts tilting towards higher temperatures as the pressure decreases. This gives rise to a reentrant phase transition, with pressure being the thermodynamic quantity that is monotonically varied, yielding a small to large and back to small black hole phase transition (as we shall later illustrate). Finally for sufficiently large tensions, , the slope of the coexistence line is always negative and does not resemble the behaviour of the liquid/gas phase transition any longer.
We also find a rather interesting limiting point in thermodynamic phase space at which the volume diverges but the entropy remains finite. We refer to black holes whose parameters are in the neighbourhood of this point as mini-entropic, since their dimensionless volume-to-area ratio 
becomes unbounded as this point is approached, contrary to the superentropic black holes  that are characterized by a ratio less than one.
The rest of our paper is organized as follows. In the next section we review the charged C-metric, discuss its thermodynamic behaviour, and look closer at the admissible parameter space of the solution, which will provide key insights as to why the swallowtail snaps. Section 3 is devoted to the study of the phase behaviour. We end with summary and conclusions in section 4.
2 Charged AdS C-metric and its thermodynamics
where we have chosen a gauge in which the electrostatic potential vanishes on the black hole horizon, and where
with being the acceleration parameter, the cosmological constant, the mass parameter and the charge parameter. The time coordinate has been rescaled by the parameter ,
determines the boundary of the AdS spacetime and the parameter encodes information about the conical deficit on the south and north poles, so that .
The metric 2.1 satisfies the Einstein equations everywhere except along the polar axes and , where there must exist a string of stress-energy in order to offset the conical deficit about these axes. This can be done by introducing cosmic strings whose tensions on the polar axes are
and are related to the conical deficits, by . Thus we have the following range for the tensions:
with the upper limit corresponding to a conical deficit of . Defining further
we can by an appropriate choice of or respectively set either of or to zero, but not both.
If the black hole has sufficiently slow acceleration (see discussion below) there will be a single (black hole) horizon. This constrains the parameter space and allows for a single temperature and a consistent thermodynamics. We turn now to consider this situation.
Before considering the conditions required for the slow acceleration, let us present the thermodynamic quantities associated with the charged accelerating black hole 
which are respectively the first law and Smarr relation.
In what follows we explicitly make the choice , so that
In other words, only one string (located at the south pole) pulls on the black hole, which is completely regular on the north pole. The first law then takes the form 4.
2.3 Parameter space
Before discussing the possible phase transitions, we must determine the admissible space of the parameters appearing in the metric 2.1 that ensure our problem is well-posed. Clearly, we have a number of conditions to impose: i) positivity of the function over the range , ii) existence of a black hole in the bulk, and iii) validity of the derived thermodynamics. The latter entails working in the slow acceleration regime 26 and 29. This ensures that is positive and that there is a single horizon whose temperature is given by its surface gravity.
In order to discuss these conditions, we introduce the new coordinates
so that the conformal boundary is situated at . We also consider the dimensionless quantities
Using these variables, and the definition of , , and , we find the following relations:
Signature of . In order to have the right metric signature , we require for . This yields
the boundaries of which give the black horizontal lines in Fig. 2.
Existence of a bulk black hole. Demanding that the spacetime admits a black hole and not a naked singularity, we require that a horizon exists in the bulk, that is has at least one root in the range preserving the signature for . To find this we can appeal to the condition for an extremal black hole
or in other words, that has a double root , corresponding to the coincidence of the inner and outer black hole horizons. Solving these two equations yields and , which can be plotted parametrically in terms of for a fixed . The resultant curve provides a lower bound for the existence of the black hole, and is displayed in Fig. 2b by the red line, denoting the extremal limit. Above this line, a black hole (with two horizons) is present, whereas no black hole exists below it.
Validity of thermodynamics. To ensure that the thermodynamic quantities 14 are well defined, it is necessary to have , which in turn imposes
The boundary is displayed in Fig. 2 by the vertical green lines.
On the other hand, the sufficient condition for the slow acceleration regime is that does not develop any roots on the boundary (neither acceleration nor cosmological horizons are present ). Since the conformal boundary is situated at , the metric function develops a root on the boundary when
for some . This yields the following relations:
The corresponding parameter space can be plotted parametrically, for ; it corresponds to the blue curves forming the right-hand boundaries of the admissible regions in Fig. 2.
Note that the condition for which the thermodynamic quantities 14 are well defined functions is weaker than the requirement of the slow acceleration regime—the blue curve cuts away an additional piece of the admissible region of the parameter space. One might suspect that the thermodynamic quantities in this removed region would correspond to the characteristics of a rapidly accelerating black hole. Even if so, the phase transition interpretation in this regime would be questionable as there are additional horizons present in the spacetime. We note, however, that a proposal  to treat additional horizons (in that case de Sitter) as ‘independent thermodynamic systems’ that do not apriori affect the phase transitions due to the black hole horizon has been recently put forward.
Point and a summary of constraints. The above constraints dictate the admissible parameter space in the dimensionless plane. Two dimensional slices of this three-dimensional parameter space can easily be displayed; see Fig. 2 for two examples of : (left) and (right). The full admissible parameter region is a union of such slices.
For a non-trivial we note the presence of a ‘point ’, the only point where the line forms the boundary of the admissible region. As we shall see this point plays a crucial role for the existence of snapping swallowtails. Point is characterized by the intersection of the following three curves: the curve, the extremal black hole curve, and the slow acceleration curve. Since the intersection of any two is sufficient for finding , this point is for example given by
The definition of and then gives
with the latter equivalent to the critical pressure, 5,
As increases the point X ‘travels upwards’ and the admissible parameter region shrinks, until at a maximum value the whole parameter space shrinks to one point. This occurs when all boundary curves intersect, that is for
For larger there is no physically admissible region. Hence is constrained to the range , which in turn implies that the mass . We note that these ranges imply that only the upper formula in 24 and the plus sign in 29 are applicable.
2.4 Mini-entropic black holes
The point , characterized above by 30 and 2.3–33, would correspond, via 14–18, to a black hole of vanishing mass but finite radius and entropy, as well as infinite volume, and potential.111 Note that the formula 2.3 admits a smooth limit , in which case we recover , corresponding to empty AdS space. Of course, this object cannot actually be physically realized since lies outside of the admissible region in parameter space (and thence the above stated thermodynamics does not apply). However it is possible to come arbitrarily close to it, for example following the slices of constant charge, pressure, and string tension, as displayed in Fig. 3 above.
From the perspective of the reverse isoperimetric inequality , black holes in the vicinity of the point are mini-entropic: their volume diverges and their area is finite as is approached, implying the dimensionless ratio in 6 diverges. This is in contrast to super-entropic black holes , whose entropy exceeds the maximum implied by the black hole volume ().
3 Phase transitions
As per usual, to uncover the thermodynamic behaviour of the system, we study the free energy, which is now also a function of the string tension ,
Thermodynamic equilibrium corresponds to the global minimum of . Non-analytic behaviour of this minimum indicates the presence of phase transitions.
3.1 Snapping swallowtails
As discussed in the introduction, charged AdS black holes without acceleration exhibit Van der Waals-like phase behaviour : for pressures one observes swallowtail behaviour of the free energy—corresponding to the first order small black hole/large black hole phase transition, as illustrated in the left part of Fig. 4. The curve is smooth for , develops a kink at , and then a swallowtail for which grows in size as pressure further decreases. For any given swallowtail, beginning at the left at , for increasing temperature the black hole has increasing radius. Following the curve rightward to its first cusp, then leftward and up to its second cusp, and then rightward again down the steeply negative slope, the radius of the black hole monotonically increases. However the global minimum of the free energy experiences a discontinuity at the intersection, at which it is thermodynamically favourable for the small black hole to undergo a first-order phase transition to a large black hole.
In the presence of acceleration the situation is much more interesting. As depicted in the right-hand diagram of Fig. 4, for small tensions and moderate pressures the swallowtail behaviour is preserved. However, contrary to the non-accelerating case, the swallowtail ceases to exist for . Instead, as decreases through , the swallowtail ‘snaps’: the small black hole branch disappears together with the extremal black hole, and re-appears as a new branch of unstable high temperature black holes (that are mini-entropic for sufficiently high temperatures). The resultant free energy diagram for is reminiscent of that of the ‘Schwarzschild-AdS’ black hole (see Fig. 5 for more details). We stress, however, that in this case no Hawking–Page transition can exist, as there is no radiation phase with non-trivial charge and non-trivial string tension .
To get an intuitive feeling as to why the swallowtail snaps, let us study the , , and ‘swallowtails’ of the free energy (displayed in Fig. 4) from a perspective of the corresponding parameter space slicing. Such curves are characterized by fixed and , and of course fixed pressure, and give rise to corresponding curves in the parameter space . In Fig. 3 we display the orthogonal projection of these curves onto a fixed plane. On one end such curves asymptote to (which would happen only for ) corresponding to the stable large black holes, on the other end they terminate either on an extremal black hole (red dashed) curve, at the point , or on the slow acceleration blue curve; in general each happening for a different value of .
When (displayed in Fig. 3 by a solid black curve) the swallowtail terminates at the point and represents the critical slice222That this slice seem to lie beyond the admissible region is simply an artifact of displaying the 2d projections of the full 3d parameter space. Since these regions get bigger as decreases, all points on the slice actually belong to the admissible region. . For the (dashed black) curve lies to the left of the critical slice and represents a true swallowtail, terminating on an extremal black hole curve at some value of . On the other hand, if the (dot-dash black) curve lies to the right of the critical slice and necessarily terminates on the slow acceleration boundary curve for some . Of course, this corresponds to the already snapped swallowtail.
Summarizing, it is the ‘crossing’ of the point in parameter space, together with the existence of the slow acceleration boundary, that is responsible for the the swallowtail snapping.
3.2 Zeroth order phase transition & bicritical point
The snap of the swallowtail at has the following rather interesting consequence illustrated in Fig. 6. As we lower the pressure through , the entire branch of stable small low temperature black holes present for disappears. Consequently for there are no longer any black holes below , with being the temperature of the upper cusp of the critical swallowtail. At the same time the global minimum of the
free energy in between and , ‘jumps upwards’ from the small black hole branch to the intermediate black hole branch, as schematically illustrated for a single black hole in Fig. 6. Here is the temperature of the bottom intersection of the critical swallowtail.
In other words, in between and we observe a zeroth-order phase transition, as the global minimum of the free energy experiences a finite jump across . Increasing the temperature from , this jump gets smaller and smaller and finally disappears at . Thus, we have a special point, at
where the coexistence line of the zeroth order phase transition characterized by and terminates and joins the first order coexistence line of the small black hole/large black hole phase transition. We call this point the bicritical point.
3.3 Phase diagrams
Having understood the free energy, we can now plot the phase diagrams, displayed for various tensions in Fig. 7. Consider first a small string tension , Fig. 7a. Similar to the non-accelerating case the diagram features the first order phase transition coexistence line (displayed by the blue curve) and the critical point (solid circle) where the first order coexistence line terminates and the transition becomes second order. A novel feature, when compared to Fig. 1, is the existence of a bicritical point (empty circle) and the associated zeroth order phase transition (red dashed curve). We also observe the existence of a no black hole region caused by the fact that low temperature black holes no longer exist below .
As the string tension increases, a region of reentrant phase transitions emerges, illustrated in Fig. 7b for . For values of in this intermediate range, the co-existence line of the first order phase transitions becomes double-valued, indicating the presence of a pressure driven reentrant phase transition, shown in greater detail in Fig. 8. As we follow the black dashed curve from the initial point of high pressure, to the final point of low pressure, we cross twice the first order coexistence line (blue curve) and once the zeroth order coexistence line (denoted by dashed red curve), undergoing a reentrant phase transition from SBH to LBH back to SBH and finally to IBH. This is the first example where reentrance is observed for black holes with the pressure as the control parameter.
Finally, for sufficiently large tensions, , the slope of the whole coexistence line becomes negative, as pressure decreases from , temperature increases instead of decreases along the line, see Fig. 7c. This transition seems very different from that of the liquid/gas phase transition.
4 Summary and conclusion
We have studied the phase behaviour of slowly accelerating charged AdS black holes, employing the recently derived thermodynamic quantities . We have found that whereas the high pressure behaviour resembles that of the non-accelerating case, there exists a second critical point at low pressures where the swallowtail snaps. We have provided an intuitive explanation of this by looking at how the swallowtail plots cut the parameter space. We can understand the snapping of the swallowtail as a result of the existence of a critical slice through the point in the parameter space, together with the existence of the slow acceleration boundary.
The coexistence line of the first order phase transition thus terminates at , where it is joined to a zeroth order coexistence line, across which we find a small to intermediate black hole phase transition. We called the point where the two coexistence lines meet a bicritical point.
We also found a new form of a reentrant phase transition from the double-valued co-existence curve, as well as a no black hole region in the plane. This is the first example of a black hole reentrant phase transition in which pressure is the parameter that montonically changes as we shift from one phase to another and then back to the first.
Finally, we have discovered the existence of (charged) mini-entropic black holes, whose temperature, electrostatic potential, and volume become unboundedly large whilst their entropy, horizon size, and mass remain finite, with the latter approaching zero. The physical properties of these objects remain to be understood.
Rotating and charged rotating black holes with non-zero acceleration are likely to yield even more interesting behaviour. Work on investigating these cases is in progress.
This work was supported in part by the Natural Sciences and Engineering Research Council of Canada. D.K. acknowledges the Perimeter Institute for Theoretical Physics for their support. Research at Perimeter Institute is supported by the Government of Canada through the Department of Innovation, Science and Economic Development Canada and by the Province of Ontario through the Ministry of Research, Innovation and Science.
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