Ehrenfest’s scheme and thermodynamic geometry in Born-Infeld AdS black holes

Ehrenfest’s scheme and thermodynamic geometry in Born-Infeld AdS black holes

Abstract

In this paper we analyze the phase transition phenomena in Born-Infeld AdS black holes using Ehrenfest’s scheme of standard thermodynamics. The critical points are marked by the divergences in the heat capacity. In order to investigate the nature of the phase transition, we analytically check both the Ehrenfest’s equations near the critical points. Our analysis reveals that this is indeed a second order phase transition. Finally, we analyze the nature of the phase transition using state space geometry approach. This is found to be compatible with the Ehrenfest’s scheme.

1 Introduction

Thermodynamics of black holes in Anti de Sitter (AdS) space has received renewed attention since the discovery of the phase transition phenomena in the Schwarzschild AdS background[1]. Till date several attempts have been made in order to describe the phase transition phenomena in black holes[2]-[11]. All these works are basically based on the fact that at the critical point(s) of phase transition the specific heat of the black hole diverges. Inspite of all these attempts, the issue regarding the classification of the nature of the phase transition in black holes remains highly debatable and worthy of further investigations. At this stage it is worthwhile to mention that in usual thermodynamics it is a general practice to adopt the Ehrenfest’s scheme[12] in order to classify the phase transition phenomena[13]-[17]. This is mainly due to two of its basic advantages namely, (i) it is simple and elegant and (ii) it provides a unique way to classify the nature of the phase transition in ordinary thermodynamic systems. Even if a phase transition is not truly a second order, we can determine the degree of its deviation by defining a new parameter called Prigogine-Defay ratio ()[13, 14, 17]. Inspired by all these facts, we propose a possible way to overcome the long standing problem regarding the classification of phase transition in black holes by incorporating the idea of Ehrenfest’s scheme from standard thermodynamics. Since black holes in many respects behave as ordinary thermodynamic objects, therefore the extension of Ehrenfest’s scheme to black hole thermodynamics seems to be quite natural. Such an attempt has been triggered very recently[18]-[23].

Constructing gravity theories in presence of various higher derivative corrections to the usual Maxwell action has been a popular topic of research for the past several years[24]-[31]. Among these non-linear theories of electrodynamics it is the Born-Infeld theory that has earned renewed attention for the past few decades due to its several remarkable features. As a matter of fact Einstein-Born-Infeld theory admits various static black hole solutions that possess several significant qualitative features which is absent in ordinary Einstein-Maxwell gravity. These are given by- (i) Depending on the value of the electric charge () and the Born-Infeld coupling parameter () it is observed that a meaningful black hole solution exists only for . On the other hand, for the corresponding extremal limit does not exist. This eventually puts a restriction on the parameter space of BI-AdS black holes[32]. This is indeed an interesting feature which is absent in the usual Einstein-Maxwell theory, (ii) Furthermore, one can note that for , which corresponds to the critical Born-Infeld-AdS (BI-AdS) case, there exists a new type of phase transition (HP3) which has identical thermodynamical features as observed during the phase transition phenomena in non-rotating BTZ black holes[32, 33]. This is also an interesting observation that essentially leads to a remarkable thermodynamical analogy which does not hold in the corresponding Reissener-Nordstom-AdS (RN-AdS) limit.

Motivated by all the above mentioned features, in the present work, we therefore aim to carry out a further investigation regarding the thermodynamic behavior of BI-AdS black holes[32],[34]-[37] in the framework of standard thermodynamics. We adopt the Ehrenfest’s scheme of usual thermodynamics in order to resolve a number of vexing issues regarding the phase transition phenomena in BI-AdS black holes. The critical points correspond to an infinite discontinuity in the specific heat (), which indicates the onset of a continuous higher order transition. At this point it is worthwhile to mention that, an attempt to verify the Ehrenfest’s equations for charged (RN-AdS) black holes was first initiated in [20]. There[20], based on numerical techniques, the authors had computed both the Ehrenfest’s equations close to the critical point(s). However, due the presence of infinite divergences in various thermodynamic entities (like, heat capacity etc.), as well as the lack of analytic techniques, at that time it was not possible to check the Ehrenfest’s equations exactly at the critical point(s). In order to address the above mentioned issues, the present paper therefore aims to provide an analytic scheme in order to check the Ehrenfest’s equations exactly at the critical point(s). Moreover, the present analysis has been generalized taking the particular example of BI-AdS black holes which is basically the non-linear generalization of RN-AdS black holes. Our analysis shows that it is indeed a second order phase transition.

Finally, we apply the widely explored state space geometry approach[38]-[39] to analyze the phase transition phenomena in BI-AdS black holes[19]-[20],[40]-[51]. Our analysis reveals that the scalar curvature () diverges exactly at the critical points where diverges. This signifies the presence of a second order phase transition, thereby vindicating our earlier analysis based on Ehrenfest’s scheme. It is also reassuring to note that, in the appropriate limit (, ) one recovers corresponding results for RN-AdS black holes[20], where is the Born-Infeld parameter and is the charge of the black hole.

Before we proceed further, let us mention about the organization of our paper. In section 2 we have discussed thermodynamics of the BI black holes in AdS space. Using Ehrenfest’s scheme, the nature of the phase transition has been discussed in section 3. In section 4 we analyze the phase transition using the (thermodynamic) state space geometry approach. Finally we draw our conclusion in section 5.

2 Thermodynamic variables of the BI-AdS black holes

In order to obtain a finite total energy for the field around a point-like charge, Born and Infeld proposed a non-linear electrodynamics[52] in 1934. The Born-Infeld black hole solution with or without a cosmological constant is a non-linear extension of the Reissner-Nordström black hole solution. In this paper we will be concerned with the Born-Infeld solution in (3+1)-dimensional AdS space-time (with a negative cosmological constant ) which is given by[32],

 ds2=−f(r)dt2+1f(r)dr2+r2dΩ2 (1)

where we have taken the gravitational constant . Here the metric coefficient is given by,

 f(r)=1−2Mr+r2+2b2r23⎛⎝1−√1+Q2b2r4⎞⎠+4Q23r2F(14,12,54,−Q2b2r4) (2)

where is the hypergeometric function[53] and is the Born-Infeld parameter. In the limit , one obtains the corresponding solution for the RN-AdS space-time. At this stage it is reassuring to note that the rest of the analysis has been carried out keeping all terms in the hyper geometric series .

The ADM mass of the black hole is defined by , which yields,

 M(r+,Q,b)=r+2+r3+2+b2r3+3(1−√1+Q2b2r4+)+2Q23r+F(14,12,54,−Q2b2r4) (3)

where is the radius of the outer horizon.

Using (2), the Hawking temperature for the BI-AdS black holes may be obtained as1,

 T = 14π(df(r)dr)r+ (4) = 14π[1r++3r++2b2r+(1−√1+Q2b2r4+)]

From the first law of black hole thermodynamics we get, . Using this we can obtain the entropy of the black hole as,

 S = ∫r+01T(∂M∂r)Qdr (5) = πr2+

Substituting (5) in (4) we can rewrite the Hawking temperature as[32],

 T=14π[√πS+3√Sπ+2b2√S√π(1−√1+Q2π2b2S2)] (6)

We can see from Figure-1 that, there is a ‘hump’ and a ‘dip’ in the graph. Another interesting thing about the graph is that, it is continuous in . This rules out the possibility of first order phase transition. In order to check whether there is a possibility of higher order phase transition, we compute the specific heat at constant potential () (which is analog of the specific heat at constant pressure () in usual thermodynamics).

The electrostatic potential difference between the black hole horizon and the infinity is defined by[35],

 Φ=Qr+F(14,12,54,−Q2b2r4+) (7)

Using (5) we may further express as,

 Φ=Q√π√SF(14,12,54,−Q2π2b2S2) (8)

From the thermodynamical relation

we find,

 (∂T∂S)Φ=(∂T∂S)Q−(∂T∂Q)S(∂Φ∂S)Q(∂Q∂Φ)S (9)

Where we have used the thermodynamic identity

 (∂Q∂S)Φ(∂S∂Φ)Q(∂Φ∂Q)S=−1. (10)

Finally using (6), (8) and (9), the heat capacity may be expressed as,

 CΦ = T(∂S∂T)Φ (11) = N(Q,b,S)D(Q,b,S)

where

 N(Q,b,S)=−2S{π+(3−2b2(−1+√1+Q2π2b2S2))S} {b2S2+(π2Q2+b2S2)F(34,1,54,−Q2π2b2S2)} (12)

and

 D(Q,b,S)=b2S2{π+(−3+2b2(−1+√1+Q2π2b2S2))S} +2b2S(−πQ+bS)(πQ+bS)F(14,12,54,−Q2π2b2S2) +(π−3S−2b2S)(π2Q2+b2S2)F(34,1,54,−Q2π2b2S2) (13)

Before going into the algebric details, let us first plot graphs (Figure (2) & Figure (3)) and make a qualitative analysis of the plots .

From these figures it is evident that the heat capacity () suffers discontinuities exactly at two points ( and ) which correspond to the critical points for the phase transition phenomena in BI-AdS black holes. Similar conclusion also follows from the plot (Figure (1)), where the ‘hump’ corresponds to and the ‘dip’ corresponds to .

The graph of shows that there are three phases of the black hole - Phase I (), Phase II () and Phase III (). Since the higher mass black hole possess larger entropy/horizon radius, therefore at we encounter a phase transition from a smaller mass black hole (phase I) to an intermediate (higher mass) black hole (phase II). On the other hand, corresponds to the critical point for the phase transition from the intermediate black hole (phase II) to a larger mass black hole (phase III). Finally, from figures (2) and (3) we also note that the heat capacity () is positive for phase I and phase III, whereas it is negative for phase II. Therefore, phase I and phase III correspond to the thermodynamically stable phases (), whereas phase II stands for a thermodynamically unstable phase ().

From the above discussions it is evident that the phase transitions we encounter in BI-AdS black holes are indeed continuous higher order. In order to address it more specifically (i.e. whether it is a second order or any higher order transition), we adopt a specific scheme, known as Ehrenfest’s scheme in standard thermodynamics.

3 Study of phase transition using Ehrenfest’s scheme

Discontinuity in the heat capacity does not always imply a seecond order transition, rather it suggests a continuous higher order transition in general. Ehrenfest’s equations play an important role in order to determine the nature of such higher order transitions for various conventional thermodynamical systems[13]-[17]. This scheme can be applied in a simple and elegant way in standard thermodynamic systems. The nature of the corresponding phase transition can also be classified by applying this scheme. Moreover, even if a phase transition is not a genuine second order, we can determine the degree of its deviation by calculating the Prigogine-Defay (PD) ratio[13, 14, 17]. Inspired by all these facts, we apply a similar technique to classify the phase transition phenomena in (BI-AdS) black holes and check the validity of Ehrenfest’s scheme for black holes.

In conventional thermodynamics, the first and the second Ehrenfest’s equations[12] are given by,

 (∂P∂T)S = 1VTCP2−CP1β2−β1=ΔCPVTΔβ (14) (∂P∂T)V = β2−β1κ2−κ1=ΔβΔκ (15)

In case of black hole thermodynamics, pressure () is replaced by the negative of the electrostatic potential difference () and volume () is replaced by charge () of the black hole.

Thus, for the black hole thermodynamics, the two Ehrenfest’s equations become[18],

 −(∂Φ∂T)S = 1QTCΦ2−CΦ1β2−β1=ΔCΦQTΔβ (16) −(∂Φ∂T)Q = β2−β1κ2−κ1=ΔβΔκ (17)

respectively. Here, the suffices 1 and 2 denote two distinct phases of the system. In addition to that, is the volume expansion coefficient and is the isothermal compressibility of the system which are defined as,

 β = 1Q(∂Q∂T)Φ (18) κ = 1Q(∂Q∂Φ)T (19)

Using (6) and (8) and considering the thermodynamic relation,

we can show that,

 β=−8b2π32S52D(Q,b,S) (20)

where the denominator was identified earlier ((13)).

In order to calculate , we make use of the thermodynamic identity,

 (∂Q∂Φ)T(∂Φ∂T)Q(∂T∂Q)Φ=−1. (21)

Using (10) we obtain from (21)

 (∂Q∂Φ)T=(∂T∂S)Q(∂Q∂Φ)S(∂T∂S)Φ (22)

Using (6), (8), (9) and (22) we finally obtain,

 κ=Ψ(Q,b,S)D(Q,b,S) (23)

where

 Ψ(Q,b,S)=−2b2S32Qπ12[2π2Q2−πS√1+Q2π2b2S2+(2b2(−1+√1+Q2π2b2S2)+3√1+Q2π2b2S2)] (24)

and the denominator is given by (13).

Note that, the denominators of both and are indeed identical with that of . This is manifested in the fact that both and diverge exactly at the point(s) where diverges (Figs. 4-7).

Being familiar with the two Ehrenfest’s equations and knowing and , we can now determine the order of the phase transition. In order to do that, we shall analytically check the validity of the two Ehrenfest’s equations at the points of discontinuity ( ). Furthermore, it should be noted that at the points of divergence, we denote the critical values for the temperature () and charge () as and respectively.

Let us now calculate the L.H.S of the first Ehrenfest’s equation (16), which may be written as,

 −[(∂Φ∂T)S]S=Si=−[(∂Φ∂Q)S]S=Si[(∂Q∂T)S]S=Si (25)

Using (6) and (8) we further obtain,

 −[(∂Φ∂T)S]S=Si=SiQi[1+(1+Q2iπ2b2S2i)F(34,1,54,−Q2iπ2b2S2i)] (26)

In order to calculate the R.H.S of the first Ehrenfest’s equation (16), we adopt the following procedure. From (11) and (18) we find,

 Qiβ = [(∂Q∂T)Φ]S=Si (27) = [(∂Q∂S)Φ]S=Si(CΦTi)

Therefore the R.H.S of (16) becomes

 ΔCΦTiQiΔβ=[(∂S∂Q)Φ]S=Si (28)

Using (8) we can further write,

 ΔCΦTiQiΔβ=SiQi[1+(1+Q2iπ2b2S2i)F(34,1,54,−Q2iπ2b2S2i)] (29)

From (26) and (29) it is evident that both the L.H.S and the R.H.S of the first Ehrenfest’s equation are indeed in good agreement at the critical points . As a matter of fact, the divergence of in the numerator is effectively cancelled out by the diverging nature of appearing at the denominator, which ultimately yields a finite value for the R.H.S of (16).

In order to calculate the L.H.S of the second Ehrenfest’s equation, we use the thermodynamic relation,

 (∂T∂Φ)Q=(∂T∂S)Φ(∂S∂Φ)Q+(∂T∂Φ)S (30)

Since diverges at the critical points (), it is evident from (11) that Also from (8) we find that has a finite value at the critical points (). Thus from (30) and using (16) we may write,

 −[(∂Φ∂T)Q]S=Si=−[(∂Φ∂T)S]S=Si=ΔCΦTiQiΔβ (31)

From (19), at the critical points we can write,

 κQi=[(∂Q∂Φ)T]S=Si (32)

Using (21) and (18) this can be further written as,

 κQi=−[(∂T∂Φ)Q]S=SiQiβ (33)

Therefore finally the R.H.S of (17) may be expressed as[22],

 ΔβΔκ = −[(∂Φ∂T)Q]S=Si (34) ≡ −[(∂Φ∂T)S]S=Si = SiQi[1+(1+Q2iπ2b2S2i)F(34,1,54,−Q2iπ2b2S2i)]

This proves the validity of the second Ehrenfest’s equation at the critical points . Finally, using (29) and (34) the Prigogine-Defay (PD) ratio[13] may be obtained as,

 Π = ΔCΦΔκTiQi(Δβ)2 (35) = 1

which confirms the second order nature of the phase transition.

4 Study of phase transition using state space geometry

The validity of the two Ehrenfest’s equations near the critical points indeed suggests a second order nature of the phase transition. In order to analyze the phase transition phenomena from a different perspective, we adopt the thermodynamic state space geometry approach[38]-[39], which has received renewed attention for the past two decades in the context of black hole thermodynamics[19]-[20],[40]-[51]. This method provides an elegant way to analyze a second order phase transition near the critical point.

In the state space geometry approach one aims to calculate the scalar curvature ()[49] which suffers a discontinuity at the critical point for the second order phase transition.

In order to calculate the curvature scalar () we need to determine the Ruppeiner metric coefficients which may be defined as[38]-[39],

 gRij=−∂2S(xi)∂xi∂xj (36)

where , , are the extensive variables of the system. From the computational point of view it is convenient to calculate the Weinhold metric coefficients[54],

 gWij=∂2M(xi)∂xi∂xj (37)

(where , ) that are conformally connected to that of the Ruppeiner geometry through the following map[40, 55]

 dS2R=dS2WT (38)

In order to calculate we choose and . Finally, using (3), the Ruppeiner metric coefficients may be found as,

 gRSQ=(−2πQS+π3Q3b2S3)⎡⎣1+3Sπ+2b2Sπ⎛⎝1−√1+Q2π2b2S2⎞⎠⎤⎦ (40)

and

 gRQQ=(4π−6π3Q25b2S2)⎡⎣1+3Sπ+2b2Sπ⎛⎝1−√1+Q2π2b2S2⎞⎠⎤⎦ (41)

Using these metric coefficients, the curvature scalar may be computed as,

 R=℘(S,Q)R(S,Q) (42)

The numerator is too much combursome which prevents us to present its detail expression for the present work. However the denominator may be expressed as,

 R=√1+π2Q2b2S2[−π+(−3+2b2(−1+√1+π2Q2b2S2))S](π2Q2+b2S2) (−π6Q6+12b2π4Q4S2−3b2π3Q2S3+b2π2Q2(9−2b2(7+3√1+π2Q2b2S2)) S4+10b4πS5+10b4(−3+2b2(−1+√1+π2Q2b2S2))S6)3 (43)

Before we conclude this section, let us note few interesting points at this stage. First of all from figures (8) and (9) we observe that the scalar curvature () diverges exactly at the points where the specific heat () diverges (also see figures (2) & (3)). This is an expected result, since according to Ruppeiner any divergence in implies a corresponding divergence in the heat capacity (which is thermodynamic analog of ) that essentially leads to a change in stability[49]. On the other hand, no divergence in could be observed at the Davis critical point[56], which is marked by the divergence in (which is the thermodynamic analog of ). Similar features have also been observed earlier[19, 20].

5 Conclusions

In this paper, based on a standard thermodynamic approach, we systematically analyze the phase transition phenomena in Born-Infeld AdS (BI-AdS) black holes. Our results are valid for all orders in the Born-Infeld (BI) parameter (). The continuous nature of the plot essentially rules out the possibility of any first order transition. On the other hand the discontinuity of the heat capacity () indicates the onset of a continuous higher order transition. In order to address this issue further, we provide a detailed analysis of the phase transition phenomena using Ehrenfest’s scheme of standard thermodynamics[12] which uniquely determines the second order nature of the phase transition. At this stage it is reassuring to note that the first application of the Ehrenfest’s scheme in order to determine the nature of phase transition in charged (Reissener-Nordstrom (RN-AdS)) AdS black holes had been commenced in [20]. There the analysis had been carried out numerically in order to check the validity of the Ehrenfest’s equations close to the critical point(s). Frankly speaking the analysis presented in [20] was actually in an underdeveloped stage. This is mainly due to the fact that at that time no such analytic scheme was available. As a result, at that stage of analysis it was not possible to check the validity of the Ehrenfest’s equations exactly at the critical point(s) due to the occurrence infinite divergences of various thermodynamic entities at the (phase) transition point(s).

In order to address the above mentioned issue, in the present article we provide an analytical scheme to check the validity of the Ehrenfest’s equations exactly at the critical point(s). Furthermore we carry out the entire analysis taking the particular example of BI-AdS black holes which is basically the non-linear generalization of RN-AdS black holes. Therefore our results are quite general and hence is valid for a wider class of charged black holes in the usual Einstein gravity.

Also, we analyze the phase transition phenomena using state space geometry approach. Our analysis shows that the scalar curvature () suffers discontinuities exactly at the (critical) points where the heat capacity () diverges. This further indicates the second order nature of the phase transition. Therefore from our analysis it is clear that both the Ehrenfest’s scheme and the state space geometry approach essentially lead to an identical conclusion. This also establishes their compatibility while studying phase transitions in black holes.

Finally, we remark that the curvature scalar, which behaves in a very suggestive way for conventional systems, displays similar properties for black holes. Specifically, a diverging curvature that signals the occurence of a second order phase transition in usual systems retains this characteristic for black holes. Our analysis reveals a direct connection between the Ehrenfest’s scheme and thermodynamic state space geometry.

Acknowledgement

The authors would like to thank the Council of Scientific and Industrial Research (C. S. I. R), Government of India, for financial support. They would also like to thank Prof. Rabin Banerjee for useful discussions.

Footnotes

1. For details regarding the properties of hyper-geometric function, see [53].

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