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Redalyc.Thermodynamic Response Functions and Maxwell Relations for a Kerr Black Hole Revista Mexicana de Física ISSN: 0035-001X [email protected] Sociedad Mexicana de Física A.C. México Escamilla, L.; Torres-Arenas, J. Thermodynamic response functions and Maxwell relations for a Kerr black hole Revista Mexicana de Física, vol. 60, núm. 1, enero-febrero, 2014, pp. 59-68 Sociedad Mexicana de Física A.C. Distrito Federal, México Available in: http://www.redalyc.org/articulo.oa?id=57029680010 How to cite Complete issue Scientific Information System More information about this article Network of Scientific Journals from Latin America, the Caribbean, Spain and Portugal Journal's homepage in redalyc.org Non-profit academic project, developed under the open access initiative RESEARCH Revista Mexicana de F´ısica 60 (2014) 59–68 JANUARY-FEBRUARY 2014 Thermodynamic response functions and Maxwell relations for a Kerr black hole L. Escamilla and J. Torres-Arenas Division´ de Ciencias e Ingenier´ıas Campus Leon,´ Universidad de Guanajuato, Loma del Bosque 103, 37150 Leon´ Guanajuato, Mexico,´ e-mail: lescamilla@fisica.ugto.mx; jtorres@fisica.ugto.mx Received 18 February 2013; accepted 4 October 2013 Assuming the existence of a fundamental thermodynamic relation, the classical thermodynamics of a black hole with mass and angular momentum is given. New definitions of the response functions and T dS equations are introduced and mathematical analogous of the Euler equation and Gibbs-Duhem relation are founded. Thermodynamic stability is studied from concavity conditions, resulting in an unstable equilibrium at all the domain except for a region of local stable equilibrium. The Maxwell relations are written, allowing to build the thermodynamic squares. Our results shown an interesting analogy between thermodynamics of gravitational and magnetic systems. Keywords: Thermodynamics; black holes; long range interactions. PACS: 05.70.-a; 04.70.Bw; 95.30.Tg 1. Introduction rem [9]. Development of the so-called black hole thermo- dynamics still continues [10–14]. Classical macroscopic thermodynamics is a branch of Existence of non-zero temperature for a black hole sup- physics of great generality, applicable to systems of elabo- ports the hypothesis that the relation between entropy and the rate structure, with different physical properties, such as me- area of the event horizon of a black hole has some physical chanical, thermal, electric and magnetic. Therefore, thermo- significance. Knowledge of this quantity makes possible to dynamics possess great importance in many fields of physics obtain the entropy of a black hole as a function of some fun- and technical sciences [1, 2]. The task of thermodynamics is damental parameters which describes such system; namely, to define suitable macroscopic quantities to describe average a thermodynamic fundamental equation for the black hole. properties of systems and explain how are these quantities Thermodynamics is used to find information about a gravita- related by means of universally valid equations. tional system composed by a black hole, approaching to the Even though thermodynamics is entirely of phenomeno- problem from the classical thermodynamics point of view [1]. logical nature, it is one of the best logically structured Although a formal study of black hole thermodynam- branches of physics. However, it is known, that the sys- ics can be explored from a more fundamental perspec- tems which interact via the so-called long-range interactions, tive [15–19], it is not the goal of this work to pursue this present non-conventional thermodynamic properties [3–5]. path. Instead, in this work exploration of the thermodynamic Gravitational, coulombic and dipolar systems, are some ex- information that can be extracted from the assumed existence amples of long-range interactions, in which it is possible to of a thermodynamic fundamental equation is considered, as observe non-common thermodynamic features, such as non- would be done for an ordinary thermodynamic system. This additivity, non-extensivity and the possibility of negative heat approach proves to be successful to recover the mathematical capacity. This work is inspired within this phenomenological structure, completely analogous, to conventional systems, in thermodynamic spirit. particular magnetic ones. Bekenstein [6,7] proposed that an appropriate multiple of This paper is organized as follows. In section two, the the event horizon area must be interpreted as the entropy, fundamental thermodynamic equation of a black hole, its nat- 3 ural parameters and the derived equations of state are briefly kBc Sbh = A; (1) discussed. The non-common features observed in these equa- 4~G tions are examined, including how can they be interpreted. where Sbh is the entropy of the black hole, kB is the Boltz- Mathematical analogous of the Euler equation and the Gibbs- mann constant, c is the speed of light in vacuum, ~ is the Duhem relation for these systems are calculated. In section Planck’s constant divided by 2¼, G is the universal constant three new response functions are defined and analyzed, in of gravity and A is the area of the event horizon. Moreover, particular, specific heat and its odd behavior is studied. With Hawking et al [8] proved that certain laws of black hole me- the aid of T dS equations, independence of the new response chanics are mathematical analogous of zeroth and first laws functions are found. In section four, the three possible Legen- of thermodynamics. Shortly after, it was proved that in addi- dre transformations are performed and the Maxwell relations tion to the laws of equilibrium thermodynamics, black holes are given. The mnemonic diagrams for those relations are obey as well, the standard theory of non-equilibrium ther- constructed (thermodynamic squares) exhibiting an interest- modynamics in the form of a fluctuation-dissipation theo- ing relation with magnetic systems. A particular application 60 L. ESCAMILLA AND J. TORRES-ARENAS of the formalism to the “rotocaloric” effect is discussed. In ones. This property is reflected in the fact that for a con- section five, stability conditions are reviewed and some con- ventional thermodynamic system, the fundamental equation sequences are analyzed. Some conclusions are given in sec- is a homogeneous first-order function of some extensive pa- tion six. rameters. Similarly, the equations of state of a conventional thermodynamic system are homogeneous zero order func- 2. The fundamental equation: Gibbs-Duhem tions. However, for the Kerr-Newman black holes, funda- mental Eq. (2), is not an homogeneous first-order function. and Euler relations Two major implications for thermodynamics systems with In this work, the simplest black holes, i.e., those with spher- this behavior arise: first, it is an indication of non-additivity; ical symmetry [20] are considered. The most general one second, non-extensivity is present, that implies that the equa- is the Kerr-Newman black hole, which is characterized by tions of state are not homogeneous zero-order functions. three parameters: mass M, angular momentum J, and elec- The fundamental cause of those particular thermody- tric charge Q. The fundamental equation in energy represen- namic properties lies in the gravitational nature of the system. tation can be found by substituting the area A(M; J; Q) in Gravitation falls in the so-called long-range interactions. It Eq. (1), using U = Mc2, and inverting the expression to get is largely known that thermodynamical description of such U = U(S; J; Q): systems presents several complications, among them, non- additivity and broken extensivity [3–5]. (Ã !"Ã !2 #)1=2 3 2 For the Kerr-Newman black holes, the equations of state ¼kBc ~cS Q U = + + J 2c2 : (2) obtained by derivation of Eq. (2), are: ~GS 2¼kB 2 Ã ! 2¼2k2 c5 J The first-order differential for the internal energy is: ­ = B ¢ §(S; J; Q); (6) Ã ! Ã ! Ã ! ~G S @U @U @U Ã ! dU = dS + dJ + dQ: (3) ¼k c4Q ¼2k2 c3Q3 @S @J @Q © = B + B ¢ §(S; J; Q); (7) J;Q S;Q S;J G ~GS In analogy with internal energy of a thermodynamic sim- Ã ! ( 2 ple system, U = U(S; V; Ni), where V stands for volume c 2 2 T = ¢ §(S; J; Q) c (~cS + ¼kBQ ) and Ni for mole number of the i-th component, partial deriva- 2GS tives appearing in Eq. (3) play the role of intensive parame- ) ters [6], c ¡ [(~cS + ¼k Q2)2 + (2¼k cJ)2] ; (8) Ã ! 2~S B B @U T ´ ; @S J;Q with §(S; J; Q) given by: Ã ! Ã ! (Ã ! @U @U 3 ­ ´ ; © ´ : (4) ¼kBc @J @Q § = S;Q S;J ~GS ) Where T is the temperature of the black hole, ­ its angular h i ¡1=2 2 2 2 velocity and © describes the electric potential for a charge Q £ (~cS + ¼kBQ ) + (2¼kBcJ) : (9) evaluated at a distance equal to the event horizon radius [21]. These relations are equivalent to the relations expressing in- Given the astrophysical relevance of the angular momentum tensive parameters in terms of the independent extensive pa- compared to the electric charge, henceforth in this work a rameters in a simple thermodynamic system, in the context Kerr black hole is considered, characterized by its mass M, of classical thermodynamics these relations are called equa- and angular momentum J. As a consequence, a fundamental tions of state, and are different than the functional relation equation U = U(S; J) by taking Q = 0 in Eq. (2) is used, between pressure and the energy density commonly used in for the sake of simplicity. the context of cosmology and gravitation, bearing the same We analyze (in natural units) the equations of state, name. T = T (S; J) and ­ = ­(S; J) by plotting each one with a The differential in Eq. (3) can be written as: fixed variable for each curve and studying its behavior. Start- dU = T dS + ­dJ + ©dQ: (5) ing with the angular velocity ­(S; J), in Fig.
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