Phase Transition of RN-AdS Black Hole with Fixed Electric Charge and Topological Charge

Lan, Shan-Quan

doi:https://doi.org/10.1155/2018/4350287

Advances in High Energy Physics

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Abstract Introduction Conclusion and Discussion Data Availability Conflicts of Interest Acknowledgments References Copyright Related Articles

Research Article | Open Access

Volume 2018 | Article ID 4350287 | https://doi.org/10.1155/2018/4350287

Phase Transition of RN-AdS Black Hole with Fixed Electric Charge and Topological Charge

Shan-Quan Lan¹

Academic Editor: Elias C. Vagenas

Received05 Sept 2018

Revised28 Oct 2018

Accepted25 Nov 2018

Published11 Dec 2018

Abstract

Phase transition of RN-AdS black hole is investigated from a new perspective. Not only is the cosmological constant treated as pressure but also the spatial curvature of black hole is treated as topological charge . We obtain the extended thermodynamic first law from which the mass is naturally viewed as enthalpy rather than internal energy. In canonical ensemble with fixed topological charge and electric charge , interesting van der Waals like oscillatory behavior in and graphs and swallow tail behavior in and graphs is observed. By applying the Maxwell equal area law and analysing the Gibbs free energy, we obtain analytical phase transition coexistence curves which are consistent with each other. The phase diagram is four dimensional with .

1. Introduction

Black hole is a simple object which can be described by only a few physical quantities, such as mass, charge, and angular momentum, while it is also a complicate thermodynamic system. Since the discovery of black hole’s entropy [1], the four-thermodynamic law [2], and the Hawking radiation [3] in 1970s, thermodynamic of black hole has become an interesting and challenging topic. Especially, in the anti-de Sitter (AdS) space, there exists Hawking-Page phase transition between stable large black hole and thermal gas [4]. Due to the AdS/CFT correspondence [5–7], the Hawking-Page phase transition is explained as the confinement/deconfinement phase transition of a gauge field [8].

When the AdS black hole is electrically charged, its thermodynamic properties become more rich. In the canonical ensemble with fixed electric charge, there is a first-order phase transition between small and large black holes [9–12]. Increasing the temperature, the phase transition coexistence curve ends at the critical point, where the first-order phase transition becomes a second-order one. In the grand canonical ensemble with fixed temperature, there is also a critical temperature. Below the critical temperature, is a single-valued function, where is electric charge and is the conjugate potential. Above the critical temperature, is a multivalued function with phase transitions [12]. The phase transition behavior of AdS black hole is reminiscent to the liquid-gas phase transition in a van der Waals system.

Viewing the cosmological constant as a dynamical pressure and the black hole volume as its conjugate quantity [13], the analogy of charged AdS black hole as a van der Waals system has been further enhanced in Ref. [14]. Both the systems share the same oscillatory behavior in pressure-volume graph and swallow tail behavior in Gibbs free energy- temperature (pressure) graph. What’s more, they have very similar phase diagrams and have exactly the same critical exponents. The phase transition property is also investigated in temperature-entropy graph [15]. Later, this analogy has been generalized to different AdS black holes, such as rotating black holes, higher dimensional black holes, Gauss-Bonnet black holes, f(R) black holes, black holes with scalar hair, etc [15–57], where more interesting phenomena are found.

Recently, the spatial curvature of electrically charged AdS black hole is viewed as variable and treated as topological charge [58, 59] in Einstein-Maxwell’s gravity and Lovelock-Maxwell theory. The authors found that the topological charge naturally arose in holography. What is more, together with all other known charges (electric charge, mass, and entropy), they satisfy an extended first law and the Gibbs-Duhem-like relation as a completeness. In our last paper [60], when the cosmological constant is not viewed as variable, we find a van der Waals type but new phase transition relating to the topological charge, while in this paper, we will treat both the cosmological constant and the spatial curvature as variables, then following one of their methods to derive the extended first law, from which one can see the cosmological constant is naturally viewed as pressure and the mass is viewed as enthalpy. Based on the extended first law, the black hole’s phase transition property will be investigated in canonical ensemble with fixed electric charge and topological charge.

This paper is organized as follows. In Section 2, following the method in Ref. [59], we will derive the extended first law in d dimensional space-time. In Section 3, by analysing the specific heat, the phase transition of AdS black hole in 4-dimensional space-time is studied and the critical point is determined. In Section 4, the van der Waals like oscillatory behavior is observed in both and graphs. Then we use the Maxwell equal area law to obtain the phase transition coexistence curve. In Section 5, the van der Waals like swallow tail behavior is observed in and graphs, then we will obtain the phase transition coexistence curve by analysing the gibbs free energy. Finally, we summarize and discuss our results in Section 6.

2. The Extended Thermodynamic First Law

The d dimensional space-time AdS black hole solutions with maximal symmetry in the Einstein-Maxwell theory arewhere are related to the ADM mass , electric charge , and cosmological constant byand is the volume of the “unit" sphere, plane, or hyperbola, and stands for the spatial curvature of the black hole. Under suitable compactifications for , we assume that the volume of the unit space is a constant hereafter [58, 59].

Following [59], the first law of thermodynamics can be derived. As the first law of thermodynamics is about the differential relation of every physical quantity, one can first find an equation containing these physical quantities and then differentiate it to obtain the first law of thermodynamics. Considering an equipotential surface with fixed (here set ), we variate both sides of the equation and obtainwhere is the radius of event horizon. Notingwe obtainMultiplying both sides with an constant factor , the above equation becomeswhere is the temperature, is the entropy, and is the electric potential. If we introduce a new “charge" as in [58, 59]then its conjugate potential is obtained as . If we define the black hole volume as , then its conjugate pressure is naturally arisen as , and the black hole mass is naturally viewed as enthalpy instead of energy. Finally, the extended first law is obtained as

3. The Specific Heat and Phase Transition

Hereafter, the investigation will be limited in dimensional space-time and in canonical ensemble with fixed electric charge and topological charge, leaving other situations for further study. First of all, we would like to analyse the behavior of the specific heat and the related possible phase transition phenomena. The first law can be rewritten in terms of energy ,So the isobaric specific heat can be written asSince we are in canonical ensemble, can be abbreviated as . From the denominator, we can conclude the following:

When , has two diverge points atwhich signals a phase transition.

When , the two diverge points of merge into one atwhich is the phase transition critical point. The critical temperature .

When , is always larger than zero, so there is no phase transition.

Comparing with the van der Waals equation, the specific volume is defined as [14]At the critical point, we obtain an interesting relationwhich is exactly the same as for the van der Waals fluid and RN-AdS black holes. Note that this number which seems to be universal does not depend on the topological charge or electric charge.

All the physical quantities can be rescaled by those at the critical point. Definingthe isobaric specific heat becomes

The behaviors of the rescaled specific heat for the cases , , and are shown in Figure 1. The curve of specific heat for has two divergent points which divide the region into three parts. Both the large radius region and the small radius region are thermodynamically stable with positive specific heat, while the medium radius region is unstable with negative specific heat. So there is a phase transition which takes place between small black hole and large black hole. The curve of specific heat for has only one divergent point and always positive denoting that is exactly the critical point. The curve of specific heat for has no divergent point and is always positive, implying that the black holes are stable and no phase transition will take place. This behavior of specific heat is very similar to that of the liquid-gas var der Waals system.

4. Oscillatory Behavior in and Graphs: Phase Transition Coexistence Curve

In the last section, we have determined the critical point and found a phase transition when . In this section and in the next section, we will derive the analytical phase transition coexistence curve by using different methods.

4.1. Maxwell Equal Area Law in Graph and Phase Transition Coexistence Curve

The temperature and entropy arewhich can be rescaled by (16) to behere . Thus we obtain

From the above equation, we can plot the curve for different in Figure 2. One can see that, for pressure , temperature curves show interesting var der Waals system’s oscillatory behavior which denote the existence of phase transition. The oscillatory part needs to be replaced by an isobar (denote as ) such that the areas above and below it are equal to each other. This treatment obeys Maxwell’s equal area law. In what follows, we will analytically determine this isobar for different .

Maxwell’s equal area law is manifest asAt points and , we have two equationsThe above three equations can be solved asThe last equation is the rescaled phase transition coexistence curve. Then we can make a backward rescale to obtain the phase transition coexistence curve,Note that the phase diagram is four dimensional (). The condition for the phase transition is that . When the topological charge , there will be no phase transition. While when the electric charge (), there will be phase transition with the critical temperature and pressure . The detailed dependence of the phase transition on the topological charge can be seen in (24) and in right graph of Figure 3.

The phase transition coexistence curves are plotted in Figure 3 for (left) and (right). The end points in the graphs are the critical points. With fixed and , the phase transition coexistence curve is reminiscent of the var der Waals system’s liquid-gas phase transition coexistence curve.

4.2. Maxwell Equal Area Law in Graph and Phase Transition Coexistence Curve

The pressure and volume arewhich can be rescaled to beThus we obtain

From the above equation, we can plot the curve for different in Figure 4. One can see that for temperature , pressure curves show interesting var der Waals system’s oscillatory behavior which corresponds to the phase transition. Similarly, the oscillatory part needs to be replaced by an isobar (denote as ) such that the areas above and below it are equal to each other. This treatment follows Maxwell’s equal area law. The analytical phase transition curve is derived as follows.

Maxwell’s equal area law is manifest asAt points and , we have two equationsThe above three equations can be solved asThe last equation is the rescaled phase transition coexistence curve, and it can be rewritten aswhich is exactly the same as (23). So the phase transition coexistence curves obtained by applying the Maxwell equal area law in graph and in graph are consistent with each other.

5. Swallow Tail Behavior in and Graphs: Phase Transition Coexistence Curve

In Section 2, we see that the black hole mass can be interpreted as enthalpy. Thus the Gibbs free energy isand its differential form in canonical ensemble can be obtained from (9)which denotes that the Gibbs free energy is a function of temperature and pressure.

Substituting black hole mass, temperature, and entropy into (32), then making a rescaling by the quantities at the critical point, we will obtainFrom the above equation, we can plot curves for different and plot curves for different in Figure 5. One can see that both panels display var der Waals system’s swallow tail behavior when and . Note that does not depend on the topological charge or the electric charge. But by applying a backward rescale, one can find that the swallow tail curves of in (34) for different and have conformal symmetry. Since phase transition takes place where the system’s two phases have equal Gibbs free energy, temperature, and pressure, the swallow tail’s intersection point is exactly the phase transition point. As a result, left panel and right panel have a duality relation and they are equal to each other. Then we will only analyse graph to derive the phase transition coexistence curve as follows.

In graph, at the phase transition point() for fixed , we assume that the black hole radius is for one phase and for the other phase. Thus we will have the following equations from (34):The above equations can be solved asThe last equation is exactly the same as (23). So the phase transition coexistence curves obtained by analysing the Gibbs free energy in graph and graph, or by applying the Maxwell equal area law in graph and graph, are consistent with each other.

6. Conclusion and Discussion

Treating the cosmological constant as a variable [13, 14] and the spatial curvature as topological charge [58, 59], thermodynamics of electrically charged Reissner-Nordstrm AdS black holes are investigated. Firstly, by variation of the equipotential equation on horizon, the extended thermodynamic first law is obtained. From the extended first law, a conjugate potential correspondent to the topological charge is arisen. Meanwhile, if the black hole volume is defined as , then its conjugate pressure is naturally assigned as the cosmological constant and the black hole mass as enthalpy.

Secondly, in four dimensional space-time and canonical ensemble with fixed electric charge and topological charge, the isobaric specific heat is calculated and the corresponding divergent solutions are derived. The two solutions merge into one at the critical point with . When , the curve of specific heat has two divergent points and is divided into three regions. The specific heat is positive for both the large radius region and the small radius region which are thermodynamically stable, while it is negative for the medium radius region which is unstable. When , the specific heat is always positive implying the black holes are stable and no phase transition will take place.

Thirdly, rescaling the quantities by those at the critical point, the behavior of temperature in graph and the behavior of pressure in graph are studied. They exhibit the interesting van de Waals gas-liquid system’s behavior. When , the curves vary monotonically and no phase transition will take place. When , the curves display an oscillatory behavior which signals phase transition. The oscillatory part is replaced by an isobar according to the Maxwell’s equal area law and the analytical phase transition coexistence curves (rescaled) are obtained which are consistent with each other. Then by making a backward rescale, the explicit phase transition coexistence curve is derive in (24) and the phase diagrams are shown in Figure 3.

Fourthly, van der Waals system’s swallow tail behavior is observed in the graph and graph when . The swallow tail’s intersection point is the phase transition point. By analytically solving the constraint equations, the rescaled phase transition coexistence curve is obtained which is consistent with those derived in graph and graph.

From the above detailed study in canonical ensemble, the analogy of RN-AdS black hole as van der Waals system has been examined when the spatial curvature is treated as topological charge and the cosmological constant is treated as pressure. Both the systems share the same oscillatory behavior and swallow tail behavior. Comparing with the case when the spatial curvature is fixed [14, 15], our phase transition diagram in Figure 3 is four dimensional (), which is more rich with an extra parameter, the topological charge.

A further investigation in grand canonical ensemble is outside the scope of this paper, but it is surely a very interesting direction for future research. The influence of this topological charge on black hole thermodynamics in other gravity theories (such as the Lovelock, Gauss-Bonnet theory, and f(R) theory) and different dimensional space-time also deserves to be disclosed in the future research. Another interesting future research line is the comparison of the influence between the electric charge and the topological charge.

In the end, we would like to point out that the black hole thermodynamics discussed in this paper is based on the first law derived from the equipotential surface with . A more conventional way to compute thermodynamics quantities is the Euclidean formalism, where the free energy is computed firstly and then the other quantities follow from it. The difference between these two formalisms remains unknown which deserves to be investigated in future.

Data Availability

The data used to support the findings of this study are included within the article.

Conflicts of Interest

The author declares that they have no conflicts of interest.

Acknowledgments

This research is supported by Department of Education of Guangdong Province, China (Grant no. 2017KQNCX124).

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Copyright

Copyright © 2018 Shan-Quan Lan. This is an open access article distributed under the Creative Commons Attribution License, which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited. The publication of this article was funded by SCOAP³.

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