Advances in High Energy Physics
Volume 2016 (2016), Article ID 1068757, 10 pages
http://dx.doi.org/10.1155/2016/1068757

Research Article

Thermodynamic Partition Function from Quantum Theory for Black Hole Horizons in Loop Quantum Gravity

Abhishek Majhi1,2

¹School of Physics, Indian Institute of Science Education and Research, Thiruvananthapuram (IISER TVM), Trivandrum 695016, India
²Astro-Particle Physics and Cosmology Division, Saha Institute of Nuclear Physics, Kolkata, India

Received 4 June 2016; Revised 16 August 2016; Accepted 30 August 2016

Academic Editor: S. Habib Mazharimousavi

Copyright © 2016 Abhishek Majhi. 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.

Abstract.

We establish the link between the thermodynamics and the quantum theory of black hole horizons through the construction of the thermodynamic partition function, partly based on some physically plausible arguments, by beginning from the description of quantum states of the horizon, considering loop quantum gravity (LQG) as the underlying theory. Although the effective “thermalized” form of the partition function has been previously used in the literature to study the effect of thermal fluctuations of the black hole horizon, nonetheless the direct link to any existing quantum theory (which is here taken to be LQG), especially a derivation of the partition function from the quantum states of the horizon, appears to be hitherto absent. This work is an attempt to bridge this small, but essential, gap that appears to be present between the existing literature of quantum theory and thermodynamics of black holes. Furthermore, it may be emphasized that this work is only concerned with the metric independent approaches to black hole thermodynamics.

1. Introduction

The thermodynamic properties associated with spacetime geometry are intimately associated with the presence of a physical horizon. In the Euclidean quantum gravity approach, it had been actually proven that the entropy of the spacetime geometry vanishes in the absence of a horizon [1]. Similarly, using certain properties of Canonical quantum gravity, within certain approximations, it has been shown that the partition function of a spacetime reduces to that of the horizon only [2, 3]. The physical significance of the presence of the horizon looks even more compelling when we find that (i) the entropy of the black hole is given by its horizon area instead of the volume of the region behind the horizon [4, 5], (ii) the thermal radiation of the black hole is emitted at the temperature which is the one associated with the horizon [6, 7], and (iii) there are laws of thermodynamics associated with the horizon [8]. All these findings compel us to think that there may be some quantum theory of the horizon geometry itself which describes the independent quantum degrees of freedom of the horizon and then only we can have a proper understanding and logical reasoning behind the emergent thermodynamic properties of the horizon manifested in its own right. The knowledge of such quantum theory of the horizon will also enable us to formulate a spacetime-metric or back ground independent horizon thermodynamics. In fact, in recent literature there have been some serious attempts to study horizon thermodynamics without referring to the bulk spacetime by constructing the partition function for the horizon only and investigating the relevant thermodynamic properties.

Thermal fluctuations of black hole horizons have been studied in various details by several authors in the recent past leading to interesting results regarding black hole thermodynamics [2, 3, 9–14]. In [2, 3, 14] thermal stability of black holes under thermal fluctuations was studied in canonical and grand canonical ensembles leading to a stability criterion for black holes which successfully explained the stabilities and instabilities of certain known black hole solutions. On the other hand, the issues of canonical and grand canonical entropy of black holes in presence of thermal fluctuations have been studied in [9–13]. The common and unique property of all these works is the use of the horizon partition function, whose construction is based on some heuristic modeling or assumptions or approximations regarding the underlying quantum structure of the horizon geometry, without referring to any classical background geometric structures, such as the metric and hence valid for arbitrary black hole horizons independent of the structure of the associated bulk spacetime. The thermodynamic properties associated with black hole horizons urge one to think of an inherent quantum description of the horizon geometry which will give rise to the notion of microstates so as to have a physical meaning of the associated entropy and hence thermality. This is the underlying physical essence of this particular statistical mechanical approach to horizon thermodynamics presented and investigated in [2, 3, 9–14].

However, none of these works [2, 3, 9–14] presents a logical straightforward derivation of the partition function based on the fundamental quantum structure of black hole horizons, which would have made the link between the microscopic quantum theory of the horizon and the associated thermodynamics as had been urged by the works in [1, 4–8]. This crucial direct link still goes begging, even though there is a well defined quantum theory for the horizon geometry present in the literature for several years [15, 16]. Perhaps the clearest quantum description of the geometry of a black hole horizon is provided by loop quantum gravity [15, 16], where the quantum degrees of freedom of the horizon belong to the Hilbert space of a quantum Chern-Simons theory coupled to point like sources (to be explained in detali later).

The theory, thus, provides a self-contained platform for the application of the statistical mechanical techniques so as to unravel the corresponding thermodynamic properties of the black hole horizon. This paper is aimed at providing a direct link between the quantum theory of horizon geometry and the associated thermodynamics through a derivation of the thermodynamic partition function associated with the horizon. This bridges the gap between the quantum geometric framework of equilibrium horizons laid down in [15, 16] and the thermodynamic aspects of the horizon studied in [2, 3, 9–14], which in turn answers the issues motivated by the works in [1, 4–8] as discussed earlier. This is precisely the important value addition of this work to the extant literature and hopefully may be of interest to the concerned readers. The structure of the paper can be debriefed as follows.

2. Equilibrium Horizon and Quantum Fluctuations: Microcanonical Ensemble

In modern day literature, a black hole horizon in gravitational and thermal equilibrium with ambient matter and radiation is described by the notion of an isolated horizon (IH) [17–19], which is a -dimensional null inner boundary of a -dimensional spacetime. An IH is a generalization of an event horizon of a stationary black hole spacetime to a more realistic scenario. As opposed to the global notion of the event horizon, an IH is defined locally, without any reference of the ambient bulk spacetime and hence can admit matter and radiation arbitrarily close to itself, whereas an event horizon cannot. The laws of black hole mechanics are completely realizable in the local framework of IH [19–21]. The mass and the surface gravity associated with the IH are also defined from a completely local perspective [19]. The strength of the IH framework is its local, background independent description in terms of the connection variables, which has led to rigorous analysis of the connection dynamics, symplectic structure, and so forth of the IH. The analysis reveals that the symplectic structure of the IH is that of an Chern-Simons (CS) theory [17, 18] (a concerned reader may look into [22] where, taking the event horizon in the Schwarzschild spacetime as an example (which is a special case of an IH), it has been shown that there is indeed an CS theory on the event horizon). In the quantum theory, the states of a QIH are given by that of the CS theory coupled to the edges of the bulk spin network which span the bulk quantum geometry and intersect the IH at specific points called punctures [15, 16].

The Hilbert space of a quantum spacetime admitting QIH as an inner boundary is given by modulo gauge transformations, where denotes bulk and denotes boundary (QIH) at a particular time slice [15, 16]. Mathematically, if the 4d spacetime admits a 3d IH as null inner boundary, then denotes a cross section of the IH [17, 18]. Hence, a generic quantum state of the spatial geometry of such a spacetime can be written as , where is the wave function corresponding to the volume or bulk states represented by an oriented graph, say , consisting of edges and vertices [23] and denotes a generic quantum state of the QIH. the Hilbert space of the CS theory coupled to the punctures made by the bulk spin network with the IH endowing them with the spin representations carried by the respective piercing edges which are solely responsible for all the relevant features of the QIH, the most important being the quantum area spectrum of the QIH. To be precise, for a given number of punctures, with spins , the QIH Hilbert space is given by where “Inv” denotes the invariance under the local gauge transformations on the QIH. Now, as it is seen that at the quantum level the full Hilbert space is the direct product space of the bulk and boundary Hilbert spaces, a generic quantum state of the QIH (boundary) can be written in terms of basis states on , independent of the bulk wave function. Hence, one should understand that a basis state of the QIH Hilbert space is actually a generic quantum state of the full Hilbert space, since the bulk part of the wave function is a linear combination of the basis states of the bulk geometry. In other words, a given spin configuration on the QIH admits all possible graphs -s) in the bulk consistent with the given configuration. This spin configurations provide the area eigenstate basis, which is the all important material in the context of QIH entropy. Such a basis state of the QIH Hilbert space is denoted by the ket . This is an eigenstate of the area operator associated with the QIH, having the area eigenvalue given by . Such a spin configuration (eigenstate) has a -fold degeneracy due to the possible arrangement of the spins yielding the same area eigenvalue. Hence, a generic quantum state of the QIH can be written as

where (say) is the probability that the QIH is found in the state .

We would like to mention that the topological structures, that is, the punctures, arise only in the quantum theory and we can consider it to be a macroscopic parameter only if we deal with an ensemble of QIHs rather than an ensemble of IHs. Thus, the Hilbert space of a QIH for a given should be appropriately written with proper designation as . But, the full Hilbert space of a classical IH designated by the corresponding CS level takes into account all possible sets of punctures [15, 16] and is given by

where

and is the Barbero-Immirzi parameter. The CS level is defined as , where is the classical area of the IH [15]. In the quantum theory, the CS coupling is an integer which is a necessary prequantization condition for the quantization of the classical IH [16]. Since we shall begin with the application of quantum mechanical ensemble theory to the QIH, the macroscopic parameters will be considered to be and [24] and the microstates resulting in the quantum degeneracy for a given and will give rise to the statistical or microcanonical entropy as a function of and [24, 25].

3. Quantum Fluctuations: The Microcanonical Ensemble

The number of microstates for a QIH with CS level and number of punctures are given by the dimension of the Hilbert space , where . The formula for the number of microstates for an arbitrary sequence of spins on number of punctures on the QIH is given by [26]

To obtain the total number of microstates of a QIH for given and , that is, the dimensionality of , we must consider all possible values of spin from to for each puncture. This is the precise argument which was provided in [24] in the other way round so as to render and to be macroscopic parameters designating a macroscopic state of a QIH that is taking the sum over all spins; the only parameters which are left bare are and . Hence we can write , where each spin is summed from to . In principle and by definition, the microcanonical entropy of the QIH is given by , where we have set the Boltzmann constant to unity. In practice [24], the calculation of is performed only approximately (the approximation is good enough in the limit which is the appropriate for QIHs with large classical area and large number of punctures) by finding the most probable distribution through the application of the method of Lagrange undetermined multipliers. The calculation has been extensively carried out in [24] and is needless to repeat here. What we shall discuss here is the physical essence of the method alongside mentioning the crucial steps of the calculation. Firstly, one can express the sum over spin values as sum over spin configurations by the application of the multinomial theorem [24]; that is,

where

This puts forward a very clear picture of the physical scenario which manifests the quantum jumps of QIH state from one area eigenstate to another, since the spin configurations are the eigenstates of the area operator of the QIH as discussed earlier. The variation of spin values all over the punctures of the QIH is the quantum fluctuations of the system. Now, any puncture can take any spin value from to with equal a priori probability and hence all the spin sequences are equally probable. But when we look at the spin configurations, the one allowing the maximum number of possible equi-probable microstates (spin sequences) that is maximally degenerate is the most probable spin configuration. Hence quantum state corresponding to the most probable configuration is the highest entropy state. At par with the basic postulates of equilibrium statistical mechanics, the degeneracy corresponding to this state overwhelmingly outnumbers the degeneracies corresponding to the other subdominant configurations which may be regarded as negligible quantum fluctuations. Thus, it is a good enough approximation to consider , where is the distribution corresponding to the most probable spin configuration and comes out to be

It may be mentioned that the classical area is related to as . It is straightforward to show that the microcanonical entropy comes out to be [24, 25]

where and are the Lagrange multipliers and we have neglected the subleading terms in the entropy [24] that are irrelevant in the present analysis. The Lagrange multipliers are solvable in terms of and from the following equations [24, 25]:

It should be noted that the most probable spin configuration is determined by the given set of values of and .

The physical essence of the microcanonical ensemble analysis is that the thermal fluctuations of the macroscopic variables are completely disallowed and what we deal with are purely quantum mechanical fluctuations of the system. It is easy to understand because we define the microcanonical ensemble by fixing the macroscopic variables, which are here and , and do not allow them to fluctuate. Thus the classically behaving macroscopic variables remain constant and the QIH jumps randomly from one quantum mechanical state to another which gives rise to the quantum uncertainty and hence the microcanonical entropy. In that sense, the resulting entropy is purely statistical. As we shall pass on to the grand canonical ensemble scenario, the effects of the thermal fluctuations will be taken into account because now the fixed macroscopic variables will be allowed to fluctuate.

Note. At this point, having known the degeneracy corresponding to given and , we can write down the canonical partition function as

and the grand canonical partition function as

where is the mean energy or the statistical mean of the Hamiltonian operator for the QIH (although the classical energy associated with the classical IH [19] has not been quantized till date, there has been a proposal of the most general possible structure of the Hamiltonian operator associated with the QIH [27, 28], which satisfies the properties of the classical energy in the correspondence limit) with given and . This is like considering several different copies of microcanonical ensembles of QIHs designated by different sets of values of and and then dealing with the effective classical behaviour of the relevant quantities, the quantum fluctuations being averaged out [29]. So (10) and (11) can be regarded as the “thermalized” forms of the quantum mechanical canonical and grand canonical partition functions, respectively, since the many-body structure of the QIH is not manifested at all in these above forms and is glossed out by the classically behaving macroscopic variables. Similar forms of the partition functions have been extensively used to investigate the thermodynamics of black holes in the IH framework previously in literature [2, 3, 9, 11–14]. However, there are several technical caveats in common which plague the approaches which also curtains some important physical issues regarding the quantum statistics and thermodynamics of black holes. In the forthcoming sections, we shall arrive at the above “thermalized” forms of the partition functions by beginning from the treatment with quantum mechanical ensembles of QIHs to get an in depth understanding of the thermodynamical issues based on the underlying quantum structures. Remarkably, albeit expectedly, the technical caveats of the earlier approaches to black hole thermodynamics get removed automatically, alongside the fact that the associated physical understandings become far more transparent, which will be discussed in detail in a separate section.

4. Thermalization: Other Quantum Mechanical Ensembles

Having reviewed the microcanonical ensemble results for a QIH, now we shall investigate the other quantum mechanical ensembles, namely, canonical and grand canonical. In the following paragraphs we shall explore in detail the construction of the canonical and grand canonical partition functions beginning from the very basic definitions and arrive at their respective “thermalized” forms.

4.1. Quantum Mechanical Canonical Partition Function

The Hilbert space structure of a QIH with given and emulates that of a gas of particles [30] in the sense that every physical phenomenon concerning a QIH is a collective many-body effect, a puncture being an individual body. It is also evident from the quantum area of QIH that is [15, 16] or the quantum energy of the QIH proposed in [27, 28]. Following this quantum “particle-like” structure of the QIH, the quantum mechanical canonical partition function can be written as

where is the quantum energy of the QIH corresponding to the spin configuration and is the energy contribution from a single puncture carrying spin and for any configuration, the total number of punctures must add up to since it is kept fixed in the canonical ensemble.

Now, from (7), considering that and are solvable in terms of and from (9a) and (9b), it is manifested that there is for every and . Thus, considering a fixed value of , a different choice of will give a different . It is then completely physical to argue that the most probable distributions corresponding to and are the closest less probable distributions corresponding to the most probable distribution for . Likewise, the other distributions in (12) are the most probable distributions for some . Thus, for fixed , in the quantum mechanical canonical ensemble, the sum over spin configurations can be replaced by sum over ; that is,

where is the temperature of the heat bath with which the QIH is considered to be in thermal contact. Since is an integer and since we deal with the large regime only the above expression can be well approximated by replacing with the summation by an integration as follows:

Equation (14) is the expression for the canonical partition function for a QIH which is suitable for studying the thermal fluctuations. This may be regarded as the “thermalized” form of the quantum mechanical canonical partition function given by (12). The information about the many-body quantum structure of the QIH is glossed by the classical behaviour of the the macroscopic variables.

4.2. Quantum Mechanical Grand Canonical Partition Function

Now, we shall allow the macroscopic variable to vary along side the energy. So, let us consider a grand canonical ensemble of QIHs where the number of punctures is now allowed to vary along side the energy. The quantum mechanical grand canonical partition function can be written as

where is the partition function for a quantum mechanical canonical ensemble of QIHs. is some fictitious parameter conjugate to the macroscopic variable , playing a role analogous to the chemical potential in case of a gas of particles. Let us rewrite (15) manifesting the many-particle structure of the QIH as

Now, we can argue in a similar way as in the case of the canonical ensemble. From (7), considering that and are solvable in terms of and from (9a) and (9b), it is manifested that there is for every and . Thus, different choices of and will give different . Based on a physical argument similar to that of the quantum mechanical canonical ensemble, in the quantum mechanical grand canonical ensemble, the sum over spin configurations can be replaced by sum over and ; that is,

are like “effective” quantum numbers for the energy and they are equispaced as they are integers. Since we are working in the large and large limits, the above discrete sum can be well approximated by replacing the summation by integration:

Equation (18) is the expression for the canonical partition function for a QIH which is suitable for studying the thermal fluctuations. This may be regarded as the “thermalized” form of the quantum mechanical grand canonical partition function given by (15). The information about the many-body quantum structure of the QIH is glossed by the classical behaviour of the the macroscopic variables.

5. The Chemical Potential: IH Thermodynamics from QIH Thermodynamics

It is worth mentioning that the most crucial consequence of all the above analysis, from the thermodynamic perspective, is that the grand canonical partition function of QIH with is the canonical partition function for IH; that is, . This is nothing surprising because looking at the structure of the full Hilbert space of an IH one would naturally consider the number of punctures to be unconserved for a given CS level . Thus, in the quantum mechanical canonical partition function of an IH, the sum over all possible quantum states underlying a classical IH implies sum over all possible spin sequences which give rise to area eigenvalues within of the classical area irrespective of the number of punctures. In fact the partition function written in [16], although in the area ensemble, takes a sum over number of punctures also. But the significance of QIH and quantum hair remained unnoticed in [16]. In that sense it is more reasonable to consider as a macroscopic variable and introduce on the first hand and then shift to the asymptotic view where the effect of the quantum hair disappears and is zero.

However, one must not confuse the analysis and the arguments regarding the chemical potential of a QIH with that of black holes having corresponding to any classical nongravitational charge, for example, Reissner-Nordstrom. One should remember that in this case there is an interplay between gravitational and nongravitational fields to attain the equilibrium. Hence, it is obvious that need not vanish to attain the equilibrium from the asymptotic viewpoint. The most important point to be noted is that one can tune the parameter from outside by controlling the nongravitational field, whereas cannot be controlled externally. The parameter actually couples a nongravitational variable to the partition function but does so in the case of which is purely (quantum) gravitational macroscopic variable. Although and appear to be playing the same role in different cases, basically they are very different as far as their physical implications are concerned. Further, has nothing to do with quantum gravity, whereas comes into play only when we consider the quantum gravity effects because the corresponding “charge” is a quantum hair [24, 30].

Finally, let us write down the IH partition function explicitly, which can be used directly to study the effects of Gaussian thermal fluctuations on the stability of a black hole [2]. The chemical potential is defined as

Thus, from the asymptotic viewpoint, as discussed above, vanishes and consequently . Now, using in (9a), one obtains

The above solution has been obtained graphically in [25] which gives the estimate . Consequently, the microcanonical entropy is then given by

One may note that now we have . Also, as a parallel consequence, using in (9b), one obtains

So, to calculate , it will not suffice to put in (18), but we also have to impose the relation between and in (22) by using a Dirac delta function, namely, . Thus, (18) now gets modified as

where we have set for convenience. Thus, we obtain the canonical partition function for the IH that is beginning from the fundamental quantum structures of the QIH. This is the same partition function which was studied in [2] and generalised to charged horizon in [3], to study the effect of Gaussian thermal fluctuations on the stability of black holes. But, as has been pointed out earlier, the derivations of the partition functions were based on some approximations and failed to establish a clear and direct link with the undelying quantum theory. One can see Appendix B for an elaborate discussion in this issue.

6. Discussion

The prime motive of the paper was the exact derivation of the horizon partition function using the fundamental quantum theory of the horizon geometry, which, we hope, has been elaborately worked out here up to a satisfactory level. The fact that the entropy of spacetime geometry vanishes in the absence of a horizon [1] strongly motivates one to think of independent quantum degrees of freedom of the horizon giving rise to the thermodynamic properties uniquely associated with the horizon; and the derivation of the thermodynamic partition function right from the scratch, which has been presented in this work, satifactorily quenches the urge by establishing the all needed direct link between the quantum and thermodynamic aspects of the horizon. Hence, the major acquisition one can have by studying this work is the logical step by step derivation of the theromodynamic partition functions of the black hole horizon based on the underlying quantum geometric framework and a clear understanding about the role of quantum and thermal fluctuations in the corresponding thermodynamics. Following this, the “thermalized” form of the partition function derived here, which was previously used in the literature to study the thermal fluctuations of the black hole horizons, now has a clear meaning and stands on the firm ground provided by the quantum geometric description of black hole horizon [15, 16]. This can be considered as an important value addition to the literature of black hole horizon thermodynamics. Apart from this, an important clarification made in this paper is that the QIH thermodynamics is delicately different from IH thermodynamics due to the role of the quantum variable which is present in the quantum scenario, but absent in the classical thermodynamic picture. In fact, by beginning from IH framework one completely misses out the essence of the underlying quantum structure, resulting in the incorporation of ad hoc assumptions and unnecessary approximations in the procedure. As has been pointed out earlier, the identification of as a macroscopic variable for QIH is the difference. Now, looking at the full Hilbert space of an IH which allows arbitrary number of punctures for a given , one may be tempted to ask that why at all shall we consider as a macroscopic variable a priori. The answer to this question may be that the Hamiltonian operator [27, 28] commutes with the number operator for punctures which renders to be a constant of motion or, in other words, apparently there is no dynamics that that can change the number of punctures. On the other hand, there is no role of at the classical level which is manifested by the absence of any term in the first law derived from the classical theory of IH [19]. Hence, it is most appropriate to begin from the study of quantum mechanical ensembles of QIHs by considering as a macroscopic variable and take the limit to arrive at the IH scenario, as shown in this paper. However, all the arguments regarding the role of in the local and asymptotic views remain at the qualitative level, the only understanding being the redshift factor as the cause of the behaviour of . A quantitative understanding of how vanishes at the asymptopia, by an LQG calculation, may bring forth some new insights. Finally, it may be pointed out that although we restrict our analysis to purely gravitational case and stop at canonical partition function of the IH, one can trivially consider nongravitational charge and extend the analysis to the grand canonical partition function of charged IHs. One can look into [3] for this extension to charged horizons. But, one must be alert that there will be tricky issues involved if one tries to generalize the analysis to rotating horizons, because we still do not have a proper quantum theory of rotating IH and this may be considered as a challenging research problem with potential consequences.

Appendix

A. Some Physical Speculations from the Chemical Potential

The chemical potential for QIH is purely of quantum origin and is absent in the classical theory. This makes the role of the chemical potential quite subtle to understand and of course very different from our usual notion of chemical potential occurring in thermodynamics of ordinary systems. It allows us to make some interesting speculations regarding the possible role of the chemical potential as far as the physical issues regarding the QIH are concerned and the possible new physics which may follow, in the following sections.

A.1. Quantum Interconversion of Geometry and Matter

In case of a system of gas of particles, we have an easy understanding of the physical meaning to the chemical potential . It governs the physical exchange of particles between the system (the gas) and the ambient reservoir, both of which are -dimensional systems. Hence, most crucially, the particles retain their identity whether in the system or in the reservoir and the scenario can be well visualized. But the scenario of QIHs is very much different. First of all the QIH is the quantum structure of the -dimensional IH, whereas the heat bath that is the exterior spacetime is -dimensional. The punctures, which are topological defects on the QIH, are describable only as long as they are on the QIH. They are not defined elsewhere off the QIH. Thus there is no possible physical reservoir of punctures with which the QIH can physically exchange punctures. In this case the reservoir in contact with the QIH carries an abstract sense. Well, it can be argued that the punctures get detached to yield open ends in the bulk quantum geometry which are often considered as matter excitations [31], but still they are not punctures which are quantum geometric excitations. The physical process in either direction is a conversion between two different objects: (i) detachment of punctures: conversion of horizon geometry to bulk matter; (ii) attachment of punctures: conversion of bulk matter to horizon geometry. Hence, the scenario of exchange of similar objects does not appear here. The very concept of “exchange” gets replaced by the concept of “conversion.” To be more precise and to make comparison (or rather distinction) between the two apparently similar scenarios we can say that the fluctuations of imply “exchange of particles” for a gas and “mutual conversion of bulk matter and horizon geometry at the quantum level” in case of a QIH. It is quite clear that in case of QIHs the physical meaning of the parameter is drastically different from that in the case of a gas of particles. The situation urges us to understand the precise quantum dynamics which converts a geometrical excitation on the horizon into an excitation of matter field in the bulk.

A.2. Quantum Topology of the Isolated Horizon: Local versus Asymptotic View

What we have been dealing with in this work is pure gravity and there is no nongravitational field in this scenario. In the LQG framework, the degrees of freedom of the QIH are completely described by CS theory coupled to the topological defects on the horizon which act as sources (topological charges) [15, 16]. The macroscopic variables and are well defined as far as LQG is concerned and are pure gravity variables. Both the dynamical and the equilibrium states of the horizon are completely governed by purely quantum gravitational effects, devoid of any nongravitational fields in this scenario. Thus, as opposed to the “tunable” potential corresponding to any nongravitational charges, the “chemical potential” of a QIH corresponding to the topological charge cannot be tuned externally. What we can do is to observe the behaviour of the parameter and understand its consequences as far as the thermodynamics of a QIH is concerned. Hence, even though we define the grand canonical partition function for a QIH by fixing and , it may happen that a particular value is allowed for the equilibrium.

At thermodynamic equilibrium, the macroscopic variables of the QIH are related by an equation of state. No matter crosses the horizon. But, even in this thermodynamic equilibrium condition a nonzero “chemical potential” that is will imply a tendency of fluctuation of about the mean value which is still dynamically present there. Since the horizon has attained equilibrium that is isolated, the area is now fixed; the fluctuations of which can now take place are only those which can keep the area fixed. A bit of thinking will allow one to realize that these fluctuations of are nothing but the changes in the quantum topology of the QIH (e.g., one puncture of area get replaced by two punctures of area ) and hence can be appropriately called quantum topological fluctuations. Thus, in spite of the fixed area at equilibrium, there will be puncture dynamics going on for a nonzero chemical potential which gives rise to the visualization of the quantum description of radiation and accretion from the horizon [32–34].

However, tracing back to the original proposal of the existence of quantum hair in [30], it should be remembered that these quantum topological fluctuations will only be observable for a local observer close to the horizon and the effects must vanish for an asymptotic observer who can only see the classical IH, the existence of punctures, and corresponding dynamics being glossed out at infinity. This explanation is supported by the fact that the first law of IH thermodynamics [19] does not contain any term as opposed to that of a QIH [30]. Thus what is observable at asymptopia is quantum topological equilibrium that is the smoothness of the topology of the horizon . Such a quantum topological equilibrium will be attained only for .

But for a local observer very close to the horizon, the quantum topological fluctuations must be observable and in that case a positive chemical potential [25] must be there which will result in a quantum topological fluctuation going on for a fixed classical area of the IH. This is like quantum dynamics underlying a classical equilibrium. The situation gives rise to the scenario that an infalling observer just before hitting the horizon will see a region of quantum fuzziness, which must be present there due to the quantum uncertainties evoked by the quantum structure of the IH. However, this explanation is provided on intuitive grounds and remains very much speculative unless one explores the scenario with LQG dynamics.

B. Value Addition to Earlier Literature: Bridging the Gap

Here we discuss the different background independent statistical mechanical approaches to black hole horizon thermodynamics that has gradually evolved step by step in literature, which will finally give us an understanding about the shortcomings of these earlier approaches and how the related technical caveats get eliminated by the present work based on the QIH framework. This will reveal the value addition of the present work to the existing literature.

As far as our knowledge is concerned, a generic statistical mechanical approach without prior use of any background metric was used to study the canonical ensemble scenario with the aim to investigate the effects of thermal fluctuations for black holes in [9–11]. The canonical partition function was written as

for a black hole (assuming in the hindsight). This is tantamount to model the quantum theory of the black hole as that of a single particle, alike the harmonic oscillator, whose energy spectrum is characterized by a single quantum number and also equispaced. Without the equispaced energy spectrum, the discrete sum cannot be approximated as an integration in any limit. The usual thermodynamic results following from the effective single particle model were applied to selected black holes and relevant conclusions were drawn. The above partition function, if not stated to be only a heuristic model, has hardly any relationship with actual black hole quantum states originating from the theory of QIH. The above model got improved a bit and some properties of QIH were incorporated in [12]. The canonical partition function was written as

considering that the energy is a function of the area of the horizon and then, assuming that all the punctures on the horizon carry spin half (neglecting the effects of other spins), the area spectrum of the horizon is made equispaced; that is, . The energy states are now characterized by a single quantum number but the energy spectrum is no more equispaced. Thus, the effective single particle model for black holes has got more generalized and for large horizons with sufficiently densely packed quantum states the discrete sum over the quantum number is replaced by an integration over a continuous variable which represents the quantum number in the continuum limit. It was only in [2] that a logical explanation of the partition function was given starting from the IH framework, albeit in a superficial approach using the tools of LQG. The partition function was no more any model but a true partition function derived from the fundamental theory of IH. But still the technical assumptions and approximations regarding the linearized area spectrum and so forth plagued the calculations resulting in the effective one-particle picture.

Similar to the canonical ensemble study of the effective one-particle model, the fluctuations of nongravitational charges were studied in the grand canonical ensemble in [11, 13], considering that the effective one particle carries a quantized charge representing the nongravitational charge of the black hole. The partition function is written as

using similar assumptions and approximations in the appropriate limits as discussed above for the canonical case, where is the chemical potential corresponding to the nongravitational charge . In [3] the partition function was derived in the IH framework, albeit in a superficial approach using the tools of LQG. The explanation of the Hamiltonian associated with the horizon was improved and the structure of the formalism was put on a stronger ground than ever. The partition function was a generic one for charged IH. But still the technical assumptions and approximations regarding the linearized area spectrum and so forth plagued the calculations resulting in the effective one-particle picture. It is worth explaining that the assumption of the linearized quantum area spectrum is tantamount to disregard the role of as an independent macroscopic parameter for QIH. Hence, the existence of the macroscopic variable at the quantum level continued to be opaqued by the assumption of the linearized quantum area spectrum.

The relevance of the many-particle nature of the QIH remained unnoticed and hence the canonical ensemble of QIHs and IHs has not been differentiated. It was in [30] that the crucial observation was made and was justified with simple reasonings in [24] that the number of punctures on the QIH should be considered to be an independent macroscopic variable which characterizes a macrostate of a QIH. Hence, it is worth investigating the crucial difference between the canonical ensemble thermodynamics of QIH and classical IH. The canonical partition function is defined for a fixed for QIH, whereas for classical IH there is no concept of . That is why the canonical partition function in (14) is tagged by the parameter , whereas there is no such tag for the canonical partition function of IH in [2]. In case of IH the canonical partition function is defined for fixed nongravitational charges [2] which are allowed to fluctuate in the corresponding grand canonical ensemble [3]. But for the QIH, the many-body quantum structure compels us to treat the complete thermodynamics in the grand canonical ensemble even in the absence of nongravitational charges.

Furthermore, there are some very important consequences of the study of the thermodynamics of the black holes beginning from the fundamental quantum structure of QIH rather than from the classical IH framework. For a canonical ensemble of IH [2] the energy is considered to be a function of area which is again assumed to be equispaced so that the summation can be replaced by integration. This assumption is severe and requires that only similar spins can be considered to be there at each puncture, preferably spin half, which is not true, although statistically spin half is the majority as found from the most probable distribution in the microcanonical ensemble. In the usual background independent approach to study the horizon thermodynamics in [2, 3, 12–14] it is considered that “the energy is a function of area.” In a precise sense, this is a very confusing statement. The statement should be made very precise; otherwise the underlying essence is not captured. Suppose one says the classical energy of an IH is the function of its classical area (or equivalently the CS level), which is fine. But this is not any sort of energy spectrum but rather the mean energy from the perspective of the QIH scenario [27, 28]. Thus the statement “equispaced area spectrum” does not have a clear meaning in the context of classical IH and hence approximations and assumptions had to be incorporated in [2, 3, 12–14].

In this work, as we begin from the very fundamental quantum structure of the IH that is the QIH framework, the physical and technical aspects of the calculations are logical and straightforward, devoid of any assumption and approximation. How the mean energy shows up in the partition function even though we begin from the quantum mechanical ensemble using the Hamiltonian operator for the QIH and hence the true energy spectrum of the same is very much transparent. Moreover, without having to make any assumption, we have the mean energy as the function of and , which are integers and hence equispaced. Thus the thermalized forms of the partition functions automatically reduce to the convenient forms which can further be approximated by replacing summation by integration.

Competing Interests

The author declares that they have no competing interests.

Acknowledgments

The author acknowledges the financial support provided by the Department of Atomic Energy of India during the initial stages of this work. The later stages of this work is funded by the Max-Planck Partner Group on Cosmology and Gravity.

References

G. W. Gibbons and S. W. Hawking, “Action integrals and partition functions in quantum gravity,” Physical Review D, vol. 15, no. 10, Article ID 2752, 1977.

P. Majumdar, “Generalized Hawking–Page phase transition,” Classical and Quantum Gravity, vol. 24, no. 7, pp. 1747–1753, 2007.

A. Majhi and P. Majumdar, “Charged quantum black holes: thermal stability criterion,” Classical and Quantum Gravity, vol. 29, no. 13, 135013, 14 pages, 2012.

J. D. Bekenstein, “Black holes and entropy,” Physical Review D, vol. 7, no. 8, p. 2333, 1973.

S. W. Hawking, “Black holes and thermodynamics,” Physical Review D, vol. 13, no. 2, pp. 191–197, 1976.

S. W. Hawking, “Particle creation by black holes,” Communications in Mathematical Physics, vol. 43, no. 3, pp. 199–220, 1975.

R. M. Wald, “On particle creation by black holes,” Communications in Mathematical Physics, vol. 45, no. 1, pp. 9–34, 1975.

J. M. Bardeen, B. Carter, and S. W. Hawking, “The four laws of black hole mechanics,” Communications in Mathematical Physics, vol. 31, pp. 161–170, 1973.

S. Das, P. Majumdar, and R. K. Bhaduri, “General logarithmic corrections to black-hole entropy,” Classical and Quantum Gravity, vol. 19, no. 9, pp. 2355–2367, 2002.

A. Chatterjee and P. Majumdar, “Black hole entropy: quantum vs thermal fluctuations,” http://arxiv.org/abs/gr-qc/0303030

G. Gour and A. J. M. Medved, “Thermal fluctuations and black-hole entropy,” Classical and Quantum Gravity, vol. 20, no. 15, pp. 3307–3326, 2003.

A. Chatterjee and P. Majumdar, “Universal canonical black hole entropy,” Physical Review Letters, vol. 92, no. 14, Article ID 141301, 2004.

A. Chatterjee and P. Majumdar, “Mass and charge fluctuations and black hole entropy,” Physical Review D, vol. 71, Article ID 024003, 2005.

A. Chatterjee and P. Majumdar, “Universal criterion for black hole stability,” Physical Review D, vol. 72, no. 4, Article ID 044005, 2005.

A. Ashtekar, J. Baez, A. Corichi, and K. Krasnov, “Quantum geometry and black hole entropy,” Physical Review Letters, vol. 80, no. 5, pp. 904–907, 1998.

A. Ashtekar, J. C. Baez, and K. Krasnov, “Quantum geometry of isolated horizons and black hole entropy,” Advances in Theoretical and Mathematical Physics, vol. 4, no. 1, pp. 1–94, 2000.

A. Ashtekar, A. Corichi, and K. Krasnov, “Isolated horizons: the classical phase space,” Advances in Theoretical and Mathematical Physics, vol. 3, no. 3, pp. 419–478, 1999.

A. Ashtekar, C. Beetle, and S. Fairhurst, “Mechanics of isolated horizons,” Classical and Quantum Gravity, vol. 17, no. 2, pp. 253–298, 2000.

A. Ashtekar, S. Fairhurst, and B. Krishnan, “Isolated horizons: hamiltonian evolution and the first law,” Physical Review D, vol. 62, no. 10, Article ID 104025, 2000.

A. Ashtekar and B. Krishnan, “Isolated and dynamical horizons and their applications,” Living Reviews in Relativity, vol. 7, p. 10, 2004.

A. Ashtekar, C. Beetle, O. Dreyer et al., “Generic isolated horizons and their applications,” Physical Review Letters, vol. 85, no. 17, pp. 3564–3567, 2000.

R. K. Kaul and P. Majumdar, “Schwarzschild horizon dynamics and SU(2) Chern-Simons theory,” Physical Review D, vol. 83, Article ID 024038, 2011.

A. Ashtekar and J. Lewandowski, “Background independent quantum gravity: a status report,” Classical and Quantum Gravity, vol. 21, no. 15, pp. R53–R152, 2004.

A. Majhi and P. Majumdar, “‘Quantum hairs’ and entropy of the quantum isolated horizon from Chern-Simons theory,” Classical and Quantum Gravity, vol. 31, no. 19, Article ID 195003, 2014.

A. Majhi, “The microcanonical entropy of quantum isolated horizon, ‘quantum hair’ N and the Barbero–Immirzi parameter fixation,” Classical and Quantum Gravity, vol. 31, no. 9, Article ID 095002, 2014.

R. K. Kaul and P. Majumdar, “Quantum black hole entropy,” Physics Letters B, vol. 439, no. 3-4, pp. 267–270, 1998.

A. Majhi, “Thermodynamics of quantum isolated horizons with model Hamiltonians,” Physical Review D, vol. 88, no. 2, Article ID 024010, 2013.

A. Majhi, “Quantum to clasical isolated horizon: energy spectrum of equilibrium black holes,” https://arxiv.org/abs/1303.4832

L. D. Landau and E. M. Lifschitz, Statistical Physics, Pergamon Press, 1980.

A. Ghosh and A. Perez, “Black hole entropy and isolated horizons thermodynamics,” Physical Review Letters, vol. 107, no. 24, Article ID 241301, 2011.

H. A. Morales-Técotl and C. Rovelli, “Fermions in quantum gravity,” Physical Review Letters, vol. 72, no. 23, pp. 3642–3645, 1994.

K. V. Krasnov, “On quantum statistical mechanics of a Schwarzschild black hole,” General Relativity and Gravitation, vol. 30, no. 1, pp. 53–68, 1998.

D. Pranzetti, “Radiation from quantum weakly dynamical horizons in loop quantum gravity,” Physical Review Letters, vol. 109, no. 1, Article ID 011301, 2012.

D. Pranzetti, “Dynamical evaporation of quantum horizons,” Classical and Quantum Gravity, vol. 30, no. 16, Article ID 165004, 2013.