Geometrothermodynamics: comments, criticisms, and support

Open Access
Regular Article - Theoretical Physics


We write explicitly the Euler identity and the Gibbs–Duhem relation for thermodynamic potentials that are not homogeneous first-order functions of their natural extensive variables. We apply the rules to the theory of geometrothermodynamics and show how the use of the natural extensive variables, instead of the modified ones, leads to misleading results. We further reveal some other ambiguities and inconsistencies in the theory and we make new suggestions.


Black Hole Thermodynamic Potential Representation Formula Conformal Factor Extensive Variable 

1 Introduction

There are a couple of theories on the geometry of thermodynamics which have been applied to black hole thermodynamics [1, 2, 3, 4, 5, 6, 7, 8]. The metrics by Weinhold [1, 2, 3, 4, 5] and Ruppeiner [6] have received criticisms for not being Legendre invariant [9]. For the Ruppeiner metric, however, this shortcoming has been remedied by proving the existence of a one-to-one correspondence between the divergences of the heat capacities and those of the curvature scalars for thermodynamic descriptions where the potentials are related to the mass (instead of the entropy) by Legendre transformations [10]. This has resulted in full agreement of the classical and the geometric descriptions of the black hole thermodynamics for most of applications met in the literature [10] and thus has corroborated the theory of the geometry of thermodynamics. While the theory by Liu et al. [7] has only received support so far [11, 12], the geometrothermodynamics (GTD) by Quevedo [9] has been subject to both criticisms [13, 14] and support [11, 12] from a physical point of view. This work presents a first criticism to GTD from a mathematical as well as a physical point of view.

Prior to this criticism, we have generalized in [15] the change of representation formula derived mostly for GTD application purposes by Quevedo et al. [16]. Such generalizations allow us to include all physical applications, particularly, applications to black hole thermodynamics, cosmology, and fluid thermodynamics.

Since this work is a series of comments and criticisms on GTD, more precisely on the conclusions derived by GTD, we assume that this theory is known to the readers and we refer to the work by Quevedo et al. [8, 9].

The remaining part of this work is divided into two sections and an Appendix. In Sect. 2 we introduce two types of extensive thermodynamic variables, the natural ones, \(E^a\), are used to express the first law of thermodynamics and the modified variables, \(E^{\,\prime a}\), in terms of which the thermodynamic potential is a homogeneous function of some order, say, \(\beta \).

The use of \(E^a\), instead of the modified extensive variables \(E^{\,\prime a}\), can lead to misleading results in GTD and any other fields [17, 18, 19, 20] where potentials which are not homogeneous first-order functions are used. We particularly show how the confusion of these sets of extensive thermodynamic variables was the source of misleading conclusions and derivations by the authors of GTD. We will also derive a generalized Euler identity, that is, an Euler identity for thermodynamic potentials that are not homogeneous first-order functions, as well as a generalized Gibbs–Duhem relation applicable to a wide range a physical problems and other useful relations. These derivations do not constitute the main purpose of this work; rather, they constitute a tool for revealing discrepancies of GTD and suggesting possible remedies.

In black hole thermodynamics the use of the modified extensive variables \(E^{\,\prime a}\) was first introduced by Davies [17]. Further developments have led to the formulation of the postulates of gravitational thermodynamics [21] where it was clearly emphasized that “fundamental equations are in general no longer homogeneous first-order functions of their extensive variables”. The analysis developed in Sect. 2, concerning the introduction of the modified extensive variables \(E^{\,\prime a}\), follows closely that presented in [17].

In Sect. 3 we comment on a series of papers by Quevedo et al. In the Appendix, we derive a useful relation, that is, the Smarr formula for Kerr black hole in \(d\)-dimensions, needed in Sect. 3.

Our main purpose in commenting on GTD and criticizing it is to provide a platform for improving the theory, which has received support from other workers as mentioned earlier in this section. In Sect. 4 we draw our conclusions concerning possible remedies to the theory.

2 Homogeneous potentials

In this work we use the convention by which repeated indices are summed except when otherwise mentioned. We use the same notations as in [8] to denote the thermodynamic quantities. This has always been the same notation in all papers on GTD. Hence (\(E^a,I^a\)) denote extensive and intensive thermodynamic variables, respectively, with \(I_a(E^a)=\partial \varPhi /\partial E^a\) (\(I_a=\delta _{ab}I^b\)) and \(\varPhi (E^a)\) is some thermodynamic potential. The first law of thermodynamics takes the form
$$\begin{aligned} \mathrm{d}\varPhi =I_a\,\mathrm{d}E^a\quad (\Sigma \text { over }a,\;a=1,2,\ldots ). \end{aligned}$$
The knowledge of \(\varPhi \) is crucial for the determination of the thermodynamic properties of the system under consideration and for its phase transitions. In classical thermodynamics, \(\varPhi \) is a homogeneous first-order function of the variables \(E^a\), which are called the natural variables [22], and the \(I^a\) are homogeneous zero-order functions of their extensive variables. The equations \(I_a(E^a)\equiv \partial \varPhi /\partial E^a\) are called equations of state.

In some thermodynamical problems [17, 18, 19, 20], including black holes, \(\varPhi \) appears to be homogeneous of some other set of extensive variables [15], denoted here by \(E^{\,\prime a}\), which is in general different from the natural set \(E^a\) in terms of which the first law (1) is formulated (as we shall see below, there are cases where \(\varPhi \) is not homogeneous at all). This is to say that in some fields of thermodynamics, \(\varPhi \) is not a homogeneous first-order function of its natural extensive variables \(E^a\), contrary to one of the postulates of classical thermodynamics.

To the best of our knowledge, in all cases of interest, particularly in black holes thermodynamics as we shall see below, the variables \(E^{\,\prime a}\) are power-law functions of \(E^a\):
$$\begin{aligned} E^{\,\prime a}=(E^a)^{p_a}\quad \text {(no summation over } a), \end{aligned}$$
where \(p_a\) depends obviously on \(a\). It was shown in [15] that \(p_a\) depends also on \(\beta \):
$$\begin{aligned} p_a\equiv p_a(\beta ), \end{aligned}$$
where \(\beta \) is the order of homogeneity of \(\varPhi \). We shall re-derive (3) in this section and show that we can always choose \(\beta =1\). In the case of (2), this means that we can always make \(\varPhi \) a homogeneous first-order function of the modified extensive variables \((E^a)^{p_a}\) instead of the natural ones \(E^a\).
Before we give some examples from black hole thermodynamics, we first consider the generic case where \(\varPhi \) is homogeneous in \(E^{\,\prime a}\) of order \(\beta \): \(\varPhi (\lambda E^{\,\prime a})=\lambda ^{\beta }\varPhi (E^{\,\prime a})\). We restrict ourselves to the case of interest (2); then by the Euler theorem we obtain
$$\begin{aligned} \beta \varPhi&= E^{\,\prime a}\frac{\partial \varPhi }{\partial E^{\,\prime a}}\quad (\Sigma \text { over }a)\end{aligned}$$
$$\begin{aligned} \quad&= \frac{E^a}{p_a}\frac{\partial \varPhi }{\partial E^a}\quad (\Sigma \text { over }a) \end{aligned}$$
where we have used \(\partial E^{\,\prime a}/\partial E^a=p_a(E^a)^{p_a-1}\) (no summation over \(a\)). Equation (5) generalizes the Euler identity to cases where the potential \(\varPhi \) fails to be homogeneous in the natural thermodynamic variables \(E^a\) in terms of which the first law (1) is formulated. Thus, in general, we have
$$\begin{aligned} \beta \varPhi \ne E^a\partial \varPhi /\partial E^a. \end{aligned}$$
We have noticed that the authors of GTD, Quevedo et al., have always assumed \(\beta \varPhi {\,\equiv \,} E^a\partial \varPhi /\partial E^a\) (or resp. \(\varPhi \propto E^a\partial \varPhi /\partial E^a\)), thus they have admitted that all \(p_a\equiv 1\) (or resp. all1 \(p_a\) are equal), which is, on the one hand, a very restrictive constraint and rarely met in black hole thermodynamics, cosmology, fluid thermodynamics or other fields of thermodynamics and, on the other hand, the constraint was applied indiscriminately to all problems the authors have tackled even when \(\varPhi \) was not homogeneous at all! We have realized that their assumption occurred in the paragraph following Eq. (37) of Ref. [8], in Eqs. (2), (4), and (11) [and probably 12] of Ref. [9], in the paragraph following Eq. (13) of Ref. [9], in Eq. (4) of Ref. [23], in the paragraph following Eq. (6) of Ref. [23], in the paragraph following Eq. (33) of Ref. [24], and in Eq. (6) of Ref. [25]; it has occurred in other related papers too as we shall see below and recently in Eq. (1) of [26].
Before we proceed with Eqs. (4) and (5), we first give an example from black hole thermodynamics. Some other examples are provided in [12, 15, 17, 27, 28]. Consider the Reissner–Nordström black hole where its mass is taken as a thermodynamic potential [29] (see also [9])
$$\begin{aligned} M=(\pi S^{-1/2}Q^2+S^{1/2})/(2\sqrt{\pi }). \end{aligned}$$
The natural extensive thermodynamic variables that enter the first law are (\(S,Q\)):
$$\begin{aligned} \mathrm{d}M=T\mathrm{d}S+\phi \mathrm{d}Q \end{aligned}$$
$$\begin{aligned} T=(\partial M/\partial S)_Q,\quad \phi =(\partial M/\partial Q)_S \end{aligned}$$
are the temperature and electric potential given by
$$\begin{aligned} T=S^{-3/2}[S-\pi Q^2]/(4\sqrt{\pi }),\;\phi =\sqrt{\pi }S^{-1/2}Q. \end{aligned}$$
Now, it is straightforward to check that \(M\) is not homogeneous in (\(S,Q\)) because it is not possible to find a real \(\beta \) such that \(M(\lambda S, \lambda Q)=\lambda ^{\beta }M(S,Q)\); rather, it is homogeneous in (\(S,Q^2\)) of order \(\beta =1/2\)
$$\begin{aligned} M(\lambda S, \lambda Q^2)=\lambda ^{\beta }M(S,Q^2) \quad \text {with }\beta =1/2 \end{aligned}$$
leading to the Euler identity (4), (5)
$$\begin{aligned} M/2&=S(\partial M/\partial S)_Q+Q^2[\partial M/\partial (Q^2)]_S\end{aligned}$$
$$\begin{aligned} \quad&=ST+Q\phi /2 \end{aligned}$$
where we have used the definitions (9) of \(T\) and \(\phi \) along with \([\partial M/\partial (Q^2)]_S=[\partial M/\partial Q]_S/(2Q)\), \(p_1\equiv p_S=1\) and \(p_2\equiv p_Q=2\). It is straightforward to check that the right-hand side of (13) is equal to \(M/2\) on substituting the expressions of \(T\) and \(\phi \) given in (10).
Now, rewriting the expression (7) of \(M\) as
$$\begin{aligned} M=[\pi (S^{\gamma })^{-1/(2\gamma )}(Q^{2\gamma })^{1/\gamma }+(S^{\gamma })^{1/(2\gamma )}]/(2\sqrt{\pi }), \end{aligned}$$
where \(\gamma >0\), one sees that the same function \(M\) is also homogeneous in (\(S^{\gamma },Q^{2\gamma }\)) of order \(\beta =(1/2)/\gamma \). For instance, if we choose \(\gamma =3\), leading to \(p_1\equiv p_S=\gamma =3\) and \(p_2\equiv p_Q=2\gamma =6\), we obtain using (5)
$$\begin{aligned} \frac{M}{6}=S^3\left( \frac{\partial M}{\partial (S^3)}\right) _Q+Q^6\left( \frac{\partial M}{\partial (Q^6)}\right) _S=\frac{ST}{3}+\frac{Q\phi }{6}, \end{aligned}$$
which is identical to (13). If one chooses \(\gamma =1/2\), the same expression (7) of \(M\) appears to be homogeneous in (\(S^{1/2},Q\)) of order \(\beta =1\) with \(p_1\equiv p_S=1/2\) and \(p_2\equiv p_Q=1\). As one sees, there is a one-to-one correspondence:
$$\begin{aligned} \text {order of homogeneity } \leftrightarrow \text { values of the } p_a\text {}. \end{aligned}$$
As a general rule: if \(f\) is homogeneous in (\(x,y,\ldots \)) of order \(\beta \), then it is also homogeneous in (\(x^{\gamma },y^{\gamma },\ldots \)) of order \(\beta /\gamma \). Since \(\gamma \) is arbitrary, this means that the order of homogeneity can be any number one chooses; one particular choice is \(\gamma =\beta \) by which \(f\) is rendered homogeneous in (\(x^{\beta },y^{\beta },\ldots \)) of order 1. This means that one can always fix the value of the order of homogeneity to 1 [15] by modifying the values of the powers \(p_a\), which depend on the order of homogeneity as we have seen in our previous example, and conversely the order of homogeneity depends on the \(p_a\).

If now \(\beta \) is some generic order of homogeneity of \(\varPhi \), it is clear that (3) holds.

Now back to (5). On dividing both sides of this equation by \(\beta \) we obtain
$$\begin{aligned} \varPhi = \frac{E^a}{\bar{p}_a}\frac{\partial \varPhi }{\partial E^a}\quad (\Sigma \text { over }a) \end{aligned}$$
where \(\bar{p}_a\equiv \beta p_a(\beta )\). Here \(\varPhi \) appears as homogeneous in \((E^a)^{\bar{p}_a}\) of order 1. Thus, the powers \(\bar{p}_a\) are those associated with an order of homogeneity equal to 1. The importance of the \(\bar{p}_a\) is that they depend neither on a particular choice of the order of homogeneity nor on the values of the \(p_a\). If a generic value \(\beta \) of the order of homogeneity is known along with the \(p_a\), as in the previous example, then
$$\begin{aligned} \bar{p}_a = \beta p_a(\beta ), \end{aligned}$$
where the right-hand side does not depend on a particular choice of \(\beta \), as this can easily be checked using the different values of the order of homogeneity in the example of the function \(M\) given by (7).
Another useful generalization is that of the Gibbs–Duhem relation, which on using (5), takes the form
$$\begin{aligned} \frac{E^a}{p_a}\,\mathrm{d}I_a=\left( \beta -\frac{1}{p_a}\right) I_a\mathrm{d}E^a \quad (\Sigma \text { over }a), \end{aligned}$$
or, equivalently, the form
$$\begin{aligned} \frac{E^a}{\bar{p}_a}\,\mathrm{d}I_a=\left( 1 -\frac{1}{\bar{p}_a}\right) I_a\mathrm{d}E^a \quad (\Sigma \text { over }a). \end{aligned}$$
One sees that only in the case where all \(\bar{p}_a\equiv 1\), the relation (20) reduces to the classical-thermodynamic Gibbs–Duhem one: \(E^a\mathrm{d}I_a=0\). In the case where all \(\bar{p}_a\) are equal but different from 1, Eq. (20) is still different from, and generalizes, the classical-thermodynamic Gibbs–Duhem relation.

3 Comments and criticisms

We now see some of the consequences of the above-mentioned assumption and give our first example of misleading results in GTD where Quevedo et al. assumed that \(E^a\partial \varPhi /\partial E^a\) is proportional to \(\varPhi \) when, according to (6) or (17), it is not.

3.1 Reissner–Nordström black holes in \(d\)-dimensions

Consider Eq. (20) of [8], which we rewrite setting
$$\begin{aligned} D\equiv (d-3)/(d-2) \end{aligned}$$
$$\begin{aligned} H(S,\phi )=-S^D\!(2D\phi ^2\!-1)/2=-S^D\mathcal {B}_3/[2(d-2)\!] \end{aligned}$$
where the correct expression of \(\phi \) is
$$\begin{aligned} \phi =Q/(2DS^D) \end{aligned}$$
instead of \(\phi =Q/(2DS^{1/D})\) as given in Eq. (13) of [8] and the temperature is such that
$$\begin{aligned} T\propto (2DS^{2D}-Q^2). \end{aligned}$$
The extremal black hole of this \(d\)-dimensional Reissner–Nordström solution corresponds to (see Eqs. (13) and (14) of [8])
$$\begin{aligned} Q^2=2DM^2,\;Q^2=2DS^{2D},\;T\equiv 0. \end{aligned}$$
According to Eqs. (8) and (34) of [8], the coefficient
$$\begin{aligned} \mathcal {A}_3=(6d-14)\phi ^2-(d-2) \end{aligned}$$
is proportional to \(S(\partial H/\partial S)_{\phi }+\phi (\partial H/\partial \phi )_{S}\). Since the authors of [8] assumed, in the paragraph following Eq. (37) of [8], that \(S(\partial H/\partial S)_{\phi }+\phi (\partial H/\partial \phi )_{S}\propto H\), they concluded that the right-hand sides in (22) and (26) are proportional, which resulted in \(H=0\Leftrightarrow \mathcal {A}_3=0\). First of all, this is not possible, since \(H=0\) (or \(\mathcal {B}_3=0\) and \(S\ne 0\)), results in \(\phi ^2=1/(2D)\) leading to \(\mathcal {A}_3=2(d-1)/D\ne 0\). Second, \(H\) as given in (22) is not homogeneous in (\(S,\phi \)) nor is it homogeneous in (\(S^r,\phi ^t\)) for all \(r\ne 0\) and \(t\ne 0\), for it is not possible to find \(r\ne 0\) and \(t\ne 0\) such that \(H(\lambda S^r,\lambda \phi ^t)=\lambda ^{\beta }H(S^r,\phi ^t)\).

We see that \(H=0\) (\(\mathcal {B}_3=0\)) leads to \(\phi ^2=1/(2D)\) or, using (23), to \(S^{2D}=Q^2/(2D)\), which is the extremal black hole (25) where the temperature (24) vanishes but \(\mathcal {A}_3\ne 0\). Thus, the conclusion drawn in the paragraph following Eq. (37) of [8], asserting that \(g_H^{II}\) is singular, is not valid; rather, the metric \(g_H^{II}\) (Eq. (34) of [8]) is not singular or degenerate in the extremal black hole limit since \(\det g_H^{II}\ne 0\).

We conclude that the scalar curvature diverges for \(H=0\) (Eq. (35) of [8]) while the metric \(g_H^{II}\) remains regular. This should signal, according to GTD itself (see the paragraph following Eq. (6) of [8]), a second order phase transition while the thermodynamic classical description asserts no phase transition in this case (see the paragraph following Eq. (21) of [8]). This discrepancy (1) constitutes a failure to describe the case \(\varPhi =H\) by GTD or (2) may lead one to modify the form of the metric \(g^{II}\) in Eq. (8) of [8]. One should also question the thermodynamic classical treatment performed in [8] in the case \(\varPhi =H\). However, we verify that the discrepancy persists.

3.2 Charged and rotating black holes

Another instance of misleading result in GTD occurred in the paragraph following Eq. (13) of [9] where the misleading equation \(\beta M=TS+\Omega _HJ+\phi Q\) was used to justify the presence of the factor \(M\) in Eq. (11) of [9]. By writing this, the authors have thus assumed that all \(p_a\) are equal without, however, fixing the value of \(\beta \).

The correct equation is \(M/2=TS+\Omega _HJ+\phi Q/2\) (see Eqs. (2.6) to (2.9) of [17]), thus the conformal factor present in Eq. (11) of [9], \(TS+\Omega _HJ+\phi Q\), is rather proportional to \(M+\phi Q\) and not to \(M\).

As is clear from the two previous examples, the authors of GTD have always treated equally the natural extensive variables (\(E^a\)) expressing the first law and the modified extensive variables (\(E^{\,\prime a}\)) in which the potential is homogeneous: Whenever they deal with a thermodynamic potential of some number of variables, \(f(x,y,z,\ldots )\), they write \(\beta f=x\partial f/\partial x+y\partial f/\partial y+\cdots \) or \(f\propto x\partial f/\partial x+y\partial f/\partial y+\cdots \) even if \(f\) is not homogeneous as in (22). In black hole thermodynamics, the shape of the Euler identity, which is not fixed a priori, is determined only once the explicit mathematical expression of \(f(x,y,z,\ldots )\) is known.

3.3 Kerr black holes in \(d\)-dimensions

A final point in our comments is the following, rather interesting, example.

First consider Eq. (47) of [8] (Kerr black hole in \(d\)-dimensions):
$$\begin{aligned} g_S^{II}=-\frac{M-\Omega J}{T^2(TS+\Omega J)}\,g_M^{II}. \end{aligned}$$
This last equation is a straightforward application of the change of representation formula, Eq. (53) of [16], which was derived by the authors of GTD taking \(\beta =1\) and all \(p_a\equiv 1\) (see Eq. (34) of [16]):
$$\begin{aligned} g^{E^{(i)}}=-\left[ I_{(i)}^{-1}E^{(i)}\frac{1}{I_aE^a}\right] g^{\varPhi } \quad [\Sigma \text { over }a,\text { no }\Sigma \text { over }(i)]. \end{aligned}$$
We stress that the realm of applicability of the change of the representation formula (28) is restricted by the constraints \(\beta =1\) and all \(p_a\equiv 1\) the authors have imposed. For instance, Eq. (28) does not apply to cases where all \(p_a\) are equal but all different from 1. As shown in the Appendix, this is precisely the case of Kerr black holes in \(d\)-dimensions.
Now back to Kerr black holes in \(d\)-dimensions. The authors of [8] obtained (27) from (28) on substituting: \(E^{(i)}=S\), \(\varPhi =M\), \(I_{(i)}=T\), \(I_aE^a=TS+\Omega J\), \(g^{E^{(i)}}=g_S^{II}\), and \(g^{\varPhi }=g_M^{II}\). This is an inappropriate application of (28), since the authors did not check whether all \(\bar{p}_a\) are equal to 1. To show that explicitly, note that the direct substitution of \(E^{(i)}=S\), \(\varPhi =M\), \(I_{(i)}=T\), \(I_aE^a=TS+\Omega J\), \(g^{E^{(i)}}=g_S^{II}\), and \(g^{\varPhi }=g_M^{II}\) in (28) yields the same expression as (27) but with \(ST\) in the numerator instead of \(M-\Omega J\):
$$\begin{aligned} g_S^{II}=-\frac{ST}{T^2(TS+\Omega J)}\,g_M^{II}. \end{aligned}$$
To reduce (29) to (27), the authors have assumed \(M(S,J)=TS+\Omega J\;[=(\partial M/\partial S)S+(\partial M/\partial J)J]\), thus taking \(\beta =1\) and all \(p_a\equiv 1\) for Kerr black holes in \(d\)-dimensions. Where does such a formula, \(M(S,J)=TS+\Omega J\), come from?2 According to the second paragraph following Eq. (15) and [15], we can always choose \(\beta =1\) but once this is done, as we shall see also in the Appendix, all \(p_a\) acquire well fixed values [Eqs. (3), (37)] that are functions of the parameters of the problem.
Moreover, it is straightforward to check that \(M(S,J)=TS+\Omega J\) is not correct by evaluating its right-hand side using the expressions of \(T(=\partial M/\partial S)\) and \(\Omega (=\partial M/\partial J)\) given in Eq. (42) of [8], then comparing the result with the expression of \(M\) given in Eq. (41) of [8]. Rather, the correct expression is (see the Appendix):
$$\begin{aligned} DM(S,J)=TS+\Omega J, \end{aligned}$$
which reduces to Eq. (2.9) of [17] (with \(Q=0\)) if \(d=4\) [\(\Rightarrow D=1/2\) by (21)].

As shown in the Appendix, and as is obvious from (30), \(M(S,J)\) is homogeneous in (\(S^D,J^D\)) of order 1 or homogeneous in (\(S,J\)) of order \(D\). We will work with the former option. But, with \(\beta =1\), \(p_1=p_S=D\ne 1\), and \(p_2=p_J=D\ne 1\), so we cannot use (28), which was derived assuming \(\beta =1\) and all \(p_a\equiv 1\) (see Eq. (34) of [16]).

We first had to generalize (28) to include the case where \(p_a\ne 1\) [15]. Thus, if the order of homogeneity is chosen equal 1 and all or some \(\bar{p}_a\ne 1\), then [15]
$$\begin{aligned} g^{E^{(i)}}&= -\frac{\varPhi \!-\!\sum _{j\ne i}I_jE^j\!+\!\sum _{j\ne i}(\bar{p}_{(i)}^{\ -1}\!-\!\bar{p}_j^{\ -1})I_jE^j}{I_{(i)}^2(I_aE^a)}\,g^{\varPhi }, \nonumber \\&\left[ \Sigma \text { over }a,\;(i)\text { fixed}\right] . \end{aligned}$$
where \(\bar{p}_a\) are the values of the \(p_a\) corresponding to an order of homogeneity equal 1 [see Eq. (18)], \(\sum _{j\ne i}I_jE^j=I_aE^a-I_{(i)}E^{(i)}\) and \(\varPhi \) is given by (17) [or by (5) on setting \(\beta =1\) and \(p_a=\bar{p}_a\)]: \(\varPhi =I_{(i)}E^{(i)}/\bar{p}_{(i)}+\sum _{j\ne i}I_jE^j/\bar{p}_j\).
Applying (31) to Kerr black holes in \(d\)-dimensions with
$$\begin{aligned}&\text {all } \bar{p}_a=D,\quad (\bar{p}_{(i)}=D, \;\bar{p}_j=D),\\&E^{(i)}=S,\; I_{(i)}=T,\; I_aE^a=TS+\Omega J,\; \sum _{j\ne i}I_jE^j=\Omega J,\\&\varPhi =(TS+\Omega J)/D=M\; [\text {see (30)}],\\&g^{E^{(i)}}=g_S^{II},\; g^{\varPhi }=g_M^{II}, \end{aligned}$$
we obtain
$$\begin{aligned} g_S^{II}=-\frac{M-\Omega J}{T^2(TS+\Omega J)}\,g_M^{II}, \end{aligned}$$
which is Eq. (27) of this paper (Eq. (47) of [8]) that the authors of [8] have reached upon using the inappropriate formula (28) and admitting that \(M(S,J)=TS+\Omega J\) holds for Kerr black holes in \(d\)-dimensions.

The fact that the authors of [8] have reached the correct formula (32) is, as explained in the Conclusion, due to the property that all \(\bar{p}_a\) are equal. This property makes the conformal factor, \(I_aE^a=TS+\Omega J\), that the authors have chosen, proportional to \(\varPhi =M\), as Eq. (30) shows.

The case where all \(p_a\) (or \(\bar{p}_a\)) are equal is not always met (see the Appendix). Even if all \(p_a\) are equal but different from 1, formula (28) is still not valid. From this point of view, Eq. (54) of [16] and Eq. (20) of [30], where (28) has been used, are not valid because \(U(S,V)\) is not known explicitly to assert that all \(p_a\equiv 1\). In these last two references, the authors, applying inappropriately formula (28), thought of \(ST\) as \(U+PV\), thus they assumed \(U(S,V)=ST-PV\) to be a universal law, that is, \(U(S,V)\) is homogeneous in (\(S,V\)) of order 1 for all thermodynamic systems. But such a law does not even apply to an ideal gas where we have \(U=ST-PV+\mu N\) with \(N\) being the one-component particle number, \(\mu =-kT\ln (AkT/P)\) is the chemical potential, \(A\equiv (2\pi mkT/h^2)^{3/2}\), \(S=Nk\ln (A\mathrm{e}^{5/2}V/N)\), \(U=3NkT/2\), and \(kT/P=V/N\) [31].

Hence, for a general potential \(U(S,V)\), the conclusion drawn in the paragraph following Eq. (21) of [30] may no longer apply since the coefficient in Eq. (21) of [30] has a more complicated structure, which is given by Eq. (31) of the present paper. This means that, besides the ambiguities that may occur if one uses \(g_U^{II}\), as clarified in the paragraph preceding Section 4 of [30], other ambiguities may occur if one uses \(g_S^{II}\).

4 Conclusion

We have concluded that the natural extrinsic thermodynamic variables expressing the first law of thermodynamics are not the same variables as the ones in which the thermodynamic potentials are homogeneous. This makes black hole thermodynamics a bit different from the classical one. Generalizations of classical-thermodynamics laws to apply to black hole thermodynamics are, however, possible and as an example we derived the generalized Gibbs–Duhem relation and we extended the Euler identity. Other generalizations were made in [15].

The misleading results and conclusions by the authors of GTD, due to the indiscriminate use of the natural thermodynamic variables and modified ones in black hole thermodynamics, has lead us to discover and reveal some other ambiguities and inconsistencies in the theory which were never discussed in the literature:
  1. 1.

    The notion of ensembles is ambiguous in GTD.

  2. 2.

    How is the conformal factor, which appears in the metric of GTD and is usually taken as \(E^a\partial \varPhi /\partial E^a\) (\(\Sigma \) over \(a\)), related to ensembles? Is there a one-to-one relationship from the set of conformal factors to the set of ensembles? If not, and mostly this is going to be the case, there should be an equivalent relation regrouping different conformal factors into equivalent sets where a representative from each set is in a one-to-one relation with an element from the set of ensembles.

  3. 3.
    It might seem possible to solve some inconsistencies in GTD had we chosen this conformal factor proportional to \(\varPhi \), that is, of the form \((E^a/\bar{p}_a)\partial \varPhi /\partial E^a\) (\(\Sigma \) over \(a\)) if \(\varPhi \) were homogeneous. This is true for the case (c) of Sect. 3 where no inconsistency occurs since the authors of [8] have taken the conformal factor \(=\) \(E^a\partial \varPhi /\partial E^a\propto (E^a/\bar{p}_a)\partial \varPhi /\partial E^a\), which results from the fact that all \(\bar{p}_a\) are equal. However, if the conformal factor is different from \(E^a\partial \varPhi /\partial E^a\), one needs to modify the change of representation formula (31). If this factor is taken equal to \(\varPhi \), we replace \(I_aE^a\) in the denominator of (31) by \(\varPhi \), and therefore the equation becomes
    $$\begin{aligned} \frac{g^{E^{(i)}}}{g^{\varPhi }}\!=\!-\!\frac{\varPhi \!-\!\sum _{j\ne i}I_jE^j\!+\!\sum _{j\ne i}(\bar{p}_{(i)}^{\ \!-\!1}\!-\!\bar{p}_j^{\ -1})I_jE^j}{I_{(i)}^2\varPhi }.\nonumber \\ \end{aligned}$$
    Other successful choices of this factor were made by the authors of GTD [16], among which we find the form \(\xi ^a_{b} I_aE^b\). In spite of what has been done in this work, the latter choice may not be one of the appropriate choices for black hole thermodynamics, since it makes use of natural extensive thermodynamic variables instead of the modified ones. A more appropriate choice could be \(\xi ^a_{b} I_aE^b/p_b\). If this is the case, one needs to replace the factor \(\xi ^a_{b} I_aE^b\) in Eq. (20) of [15] by \(\xi ^a_{b} I_aE^b/p_b\), yielding
    $$\begin{aligned} g^{E^{(i)}}&= -\frac{1}{\beta I_{(i)}} \bigg [ \frac{\xi ^{(i)}_{(i)} E^{(i)}}{p_{(i)}} + \sum _{j\ne i}\bigg (\frac{\xi ^{(i)}_{(i)}}{p_{(i)}} - \xi ^j_{j}\beta \bigg ) \frac{I_jE^j}{I_{(i)}}\bigg ]\nonumber \\&\times \frac{g^{\varPhi }}{(\xi ^a_{b} I_aE^b/p_b)}. \end{aligned}$$
  4. 4.

    If \(\varPhi \) is not homogeneous, as in the case (a) of Sect. 3, one may consider to define this conformal factor using generalized homogeneous functions [32, 33]. Generalized homogeneous functions seem to be the most appropriate available way to define the conformal factor even if \(\varPhi \) were homogeneous. In fact, these functions introduced for the first time in [32] have the properties that their derivatives and their Legendre transforms are also generalized homogeneous functions. The latter property is not satisfied in the change of representation in GTD made in [16, Sect. IV] where it is admitted that the new representation \(E^{(i)}\) is not a homogeneous function when the old representation \(\varPhi \) is.



  1. 1.

    When all \(p_a\) are equal, it is safe to write \(\varPhi \propto E^a\partial \varPhi /\partial E^a\) but it is neither correct nor is it safe, as we shall see in case (c) of Sect. 3 concerning Kerr black holes in \(d\)-dimensions, to assume and use the equality \(\varPhi = E^a\partial \varPhi /\partial E^a\).

  2. 2.

    And where does the formula \(U(S,V)=ST-PV\), which has been used in Eq. (20) of [30], come from? Here \(U(S,V)\) is supposed to be arbitrary in [30], and thus it is not known explicitly. Such a formula is not even valid for a monatomic ideal gas with \(PV=nRT\) and \(U=3nRT/2\), for this would lead to \(S=\) constant.


  1. 1.
    F. Weinhold, Metric geometry of equilibrium thermodynamics. J. Chem. Phys. 63(6), 2479–2483 (1975)ADSCrossRefMathSciNetGoogle Scholar
  2. 2.
    F. Weinhold, Metric geometry of equilibrium thermodynamics. II. Scaling, homogeneity, and generalized Gibbs–Duhem relations. J. Chem. Phys. 63(6), 2484–2487 (1975)ADSCrossRefMathSciNetGoogle Scholar
  3. 3.
    F. Weinhold, Metric geometry of equilibrium thermodynamics. III. Elementary formal structure of a vector-algebraic representation of equilibrium thermodynamics. J. Chem. Phys. 63(6), 2488–2495 (1975)ADSCrossRefMathSciNetGoogle Scholar
  4. 4.
    F. Weinhold, Metric geometry of equilibrium thermodynamics. IV. Vector-algebraic evaluation of thermodynamic derivatives. J. Chem. Phys. 63(6), 2496–2501 (1975)ADSCrossRefMathSciNetGoogle Scholar
  5. 5.
    F. Weinhold, Metric geometry of equilibrium thermodynamics. V. Aspects of heterogeneous equilibrium. J. Chem. Phys. 65(2), 559–564 (1976)ADSCrossRefGoogle Scholar
  6. 6.
    G. Ruppeiner, Thermodynamics: a Riemannian geometric model. Phys. Rev. A 20(4), 1608–1613 (1979)ADSCrossRefGoogle Scholar
  7. 7.
    H. Liu, H. Lü, M. Luo, K.-N. Shao, Thermodynamical metrics and black hole phase transitions. JHEP 2010(12), 054 (2010). arXiv:1008.4482
  8. 8.
    A. Bravetti, D. Momeni, R. Myrzakulov, H. Quevedo, Geometrothermodynamics of higher dimensional black holes. Gen. Relativ. Gravit. 45(8), 1603–1617 (2013). arXiv:1211.7134
  9. 9.
    H. Quevedo, Geometrothermodynamics of black holes. Gen. Relativ. Gravit. 40(5), 971–984 (2008). arXiv:0704.3102
  10. 10.
    S.A. Hosseini Mansoori, B. Mirza, Correspondence of phase transition points and singularities of thermodynamic geometry of black holes. Eur. Phys. J. C 74(1), 2681 (2014). arXiv:1308.1543
  11. 11.
    M.E. Rodrigues. G.T. Marques, Thermodynamics of a class of non-asymptotically flat black holes in Einstein–Maxwell-dilaton theory. Gen. Relativ. Gravit. 45(7), 1297–1311 (2013). arXiv:1206.0763
  12. 12.
    M. Azreg-Aïnou, M.E. Rodrigues, Thermodynamical, geometrical and Poincaré methods for charged black holes in presence of quintessence. JHEP 2013(09), 146 (2013). arXiv:1211.5909
  13. 13.
    M.E. Rodrigues, Z.A.A. Oporto, Thermodynamics of phantom black holes in Einstein–Maxwell-dilaton theory. Phys. Rev. D 85(10), 104022 (2012). arXiv:1201.5337
  14. 14.
    D.F. Jardim, M.E. Rodrigues, M.J.S. Houndjo, Thermodynamics of phantom Reissner–Nordström-AdS black hole. Eur. Phys. J. Plus 127(10), 123 (2012). arXiv:1202.2830
  15. 15.
    M. Azreg-Aïnou, On the conformal metric structure of geometrothermodynamics’: generalizations. J. Math. Phys. 55(3), 033505 (2014). arXiv:1311.6595
  16. 16.
    A. Bravetti, C.S. Lopez-Monsalvo, F. Nettel, H. Quevedo, The conformal metric structure of geometrothermodynamics. J. Math. Phys. 54(3), 033513 (2013). arXiv:1302.6928
  17. 17.
    P.C.W. Davies, The thermodynamic theory of black holes. Proc. R. Soc. Lond. A 353(1675), 499–521 (1977)ADSCrossRefGoogle Scholar
  18. 18.
    G.T. Houlsby, A.M. Puzrin, Rate-dependent plasticity models derived from potential functions. J. Rheol. 46(1), 113 (2002)ADSCrossRefGoogle Scholar
  19. 19.
    M.A. Biot, Theory of stress–strain relations in anisotropic viscoelasticity and relaxation phenomena. J. Appl. Phys. 25(11), 1385 (1954)ADSCrossRefMATHGoogle Scholar
  20. 20.
    R.A. Schapery, Application of thermodynamics to thermomechanical, fracture and birefringent phenomena in viscoelastic media. J. Appl. Phys. 35(5), 1451 (1964)ADSCrossRefMathSciNetGoogle Scholar
  21. 21.
    E.A. Martinez, The postulates of gravitational thermodynamics. Phys. Rev. D 54(10), 6302 (1996)ADSCrossRefMathSciNetGoogle Scholar
  22. 22.
    E. Keszei, Chemical thermodynamics: an introduction (Springer, Berlin, 2012)CrossRefGoogle Scholar
  23. 23.
    H. Quevedo, A. Sánchez, S. Taj, A. Vázquez, Phase transitions in geometrothermodynamics. Gen. Relativ. Gravit. 43(4), 1153–1165 (2011). arXiv:1010.5599
  24. 24.
    M. Akbar, H. Quevedo, K. Saifullah, A. Sánchez, S. Taj, Thermodynamic geometry of charged rotating BTZ black holes. Phys. Rev. D 83(8), 084031 (2011). arXiv:1101.2722
  25. 25.
    H. Quevedo, A. Vázquez, The geometry of thermodynamics. AIP Conf. Proc. 977, 165–172 (2008). arXiv:0712.0868
  26. 26.
    H. Quevedo, F. Nettel, C.S. Lopez-Monsalvo, A. Bravetti, Representation invariant geometrothermodynamics: applications to ordinary thermodynamic systems. J. Geom. Phys. 81, 1–9 (2014)Google Scholar
  27. 27.
    S. Chen, B. Wang, R. Su, Hawking radiation in a d-dimensional static spherically symmetric black hole surrounded by quintessence. Phys. Rev. D 77(12), 124011 (2008). arXiv:0801.2053
  28. 28.
    R. Banerjee, B.R. Majhi, S.K. Modak, S. Samanta, Killing symmetries and Smarr formula for black holes in arbitrary dimensions. Phys. Rev. D 82(12), 124002 (2010). arXiv:1007.5204
  29. 29.
    P.C.W. Davies, Thermodynamics of black holes. Rep. Prog. Phys. 41(8), 1313–1355 (1978)ADSCrossRefGoogle Scholar
  30. 30.
    A. Bravetti, F. Nettel, Second order phase transitions and thermodynamic geometry: a general approach. arXiv:1208.0399v1 and v2
  31. 31.
    D.A. McQuarrie, Statistical physics (Harper & Row Publishres, New York, 1976)Google Scholar
  32. 32.
    A. Hankey, H.E. Stanley, Systematic application of generalized homogeneous functions to static scaling, dynamic scaling, and universality. Phys. Rev. B 6(9), 3515–3542 (1972) Google Scholar
  33. 33.
    H.E. Stanley, Introduction to phase transitions and critical phenomena (Oxford University Press, New York, 1987)Google Scholar
  34. 34.
    J.E. Åman, N. Pidokrajt, Geometry of higher-dimensional black hole thermodynamics. Phys. Rev. D 73(2), 024017 (2006). arXiv:0510139

Copyright information

© The Author(s) 2014

Open AccessThis article is distributed under the terms of the Creative Commons Attribution License which permits any use, distribution, and reproduction in any medium, provided the original author(s) and the source are credited.

Funded by SCOAP3 / License Version CC BY 4.0.

Authors and Affiliations

  1. 1.Engineering FacultyBaşkent UniversityAnkaraTurkey

Personalised recommendations