Advances in High Energy Physics

Volume 2018, Article ID 1043639, 6 pages

https://doi.org/10.1155/2018/1043639

## Thermodynamics of Charged AdS Black Holes in Rainbow Gravity

Institute of Theoretical Physics, Lanzhou University, Lanzhou 730000, China

Correspondence should be addressed to Jian-Bo Deng; nc.ude.uzl@bjgned

Received 4 June 2018; Accepted 5 December 2018; Published 18 December 2018

Guest Editor: Farook Rahaman

Copyright © 2018 Ping Li et al. 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 SCOAP^{3}.

#### Abstract

In this paper, the thermodynamic property of charged AdS black holes is studied in rainbow gravity. By the Heisenberg Uncertainty Principle and the modified dispersion relation, we obtain deformed temperature. Moreover, in rainbow gravity we calculate the heat capacity in a fixed charge and discuss the thermal stability. We also obtain a similar behaviour with the liquid-gas system in extending phase space (including and ) and study its critical behavior with the pressure given by the cosmological constant and with a fixed black hole charge . Furthermore, we study the Gibbs function and find its characteristic swallow tail behavior, which indicates the phase transition. We also find that there is a special value about the mass of test particle which would lead the black hole to zero temperature and a diverging heat capacity with a fixed charge.

#### 1. Introduction

It is known Lorentz symmetry which is one of most important symmetries in nature; however, some researches indicate that the Lorentz symmetry might be violated in the ultraviolet limit [1–5]. Since the standard energy-momentum dispersion relation relates to the Lorentz symmetry, the deformation of Lorentz symmetry would lead to the modification of energy-momentum dispersion relation. In fact, some calculations in loop quantum gravity have showed the dispersion relations may be deformed. Meanwhile, based on the deformed energy-momentum dispersion relation the double special relativity has arisen [6, 7]. In this theory, in addition to the velocity of light being the maximum velocity attainable there is another constant for maximum energy scale in nature which is the Planck energy . It gives different picture for the special relativity in microcosmic physics. The theory has been generalized to curved spacetime by Joao Magueijo and Lee Smolin, called gravity’s rainbow [8]. In their theory, the geometry of spacetime depends on the energy of the test particle and observers of different energy would see different geometry of spacetime. Hence, a family of energy-dependent metrics named rainbow metrics will describe the geometry of spacetime, which is different from general gravity theory. Based on the nonlinear of Lorentz transformation, the energy-momentum dispersion relation can be rewritten aswhere is the Planck energy. The rainbow functions and are required to satisfyIn this case, the deformed energy-momentum dispersion relation equation (1) will go back to classical one when the energy of the test particle is much lower than . Due to this energy-dependent modification to the dispersion relation, the metric in gravity’s rainbow could be rewritten as [9]where the energy dependence of the frame fields isand here the tilde quantities refer to the energy-independent frame fields. This leads to a one-parameter Einstein equationwhere and are energy-dependent Einstein tensor and energy-momentum tensor and and are energy-dependent cosmological constant and Newton constant. Generally, many forms of rainbow functions have been discussed in literatures; in this paper we will mainly employ the following rainbow functions:which has been widely used in [10–18].

Recently, Schwarzschild black holes, Schwarzschild AdS black holes, and Reissner-Nordstrom black holes in rainbow gravity [19–21] have been studied. Ahmed Farag Alia, Mir Faizald, and Mohammed M. Khalile [15] studied the deformed temperature about charged AdS black holes in rainbow gravity based on Heisenberg Uncertainty Principle (HUP), . In this paper, we study the thermodynamical property about the charged AdS black holes in rainbow gravity based on the usual HUP, . Moreover, we study how the mass of test particle influences thermodynamical property for charged AdS black holes.

The paper is organized as follows. In the next section, by using the HUP and the modified dispersion relation, we obtain deformed temperature, and we also calculate heat capacity with a fixed charge and discuss the thermal stability. In Section 3, we find the charged AdS black holes have similar behaviour with the liquid-gas system with the pressure given by the cosmological constant while we treat the black holes charge as a fixed external parameter, not a thermodynamic variable. We also calculate the Gibbs free energy and find characteristic swallow tail behavior. Finally, the conclusion and discussion will be offered in Section 4.

#### 2. The Thermal Stability

In rainbow gravity the line element of the modified charged AdS black holes can be described as [15]whereGenerally, which is cosmological constant. Because all energy dependence in the energy-independent coordinates must be in the rainbow functions and , is independent on the energy of test particle [8]. In gravity’s rainbow, the deformed temperature related to the standard temperature was [15]where is horizon radius.

In gravity’s rainbow, although the metric depends on the energy of test particle, the usual HUP can be still used [19]. For simplicity we take in the following discussion, by combining (1) with (6) we can getwhere , is the mass of test particle, and is a constant parameter.

Generally, the standard temperature was given by [22]When using (6) and (10), we can get the temperature of charged AdS black holes in rainbow gravitywhere . It is easy to find when . Equation (12) shows that there are two solutions when , one corresponds to extreme black hole and the other to . The second solution indicates the temperature of black holes completely depends on the mass of test particle when the black holes keep with fixed mass, charge, and anti-de Sitter radius. The bigger the mass of test particle is, the smaller the temperature of black holes is. When , the temperature keeps zero. Generally, due to gravity’s rainbow, a minimum radius with respect to the black hole is given and is related to a radius of black hole remnant when the temperature tends to zero [15]. However, our paper shows all black holes can keep zero temperature when the test particle mass approaches a value, such as . But due to in general condition, it may be difficult to test the phenomenon with zero temperature about black holes.

In general, the thermal stability can be determined by the heat capacity, which is also used to the systems of black holes [17, 23–25]. In other words, the positive heat capacity corresponds to a stable state and the negative heat capacity corresponds to unstable state. In following discussions, we will focus on the heat capacity to discuss the stability of black holes. When , the mass of charged AdS black holes can be calculated asBased on the first law with the deformed temperature [20], the modified entropy can be computedNote that the next leading order is logarithmic as , which is similar to the quantum correction in [26–31]. With we can get . We can find the result is in agreement with the standard entropy when , which is standard condition.

The heat capacity with a fixed charge can be calculated aswhich shows that reduces to standard condition [22] with . Obviously, the heat capacity is diverging when . Generally, when the temperature vanishes, the heat capacity also tends to zero. However, our paper shows a different and anomalous phenomenon. Fortunately, the phenomenon is just an observation effect; the result gives us a way to test the theory of rainbow gravity. Some of the conditions above indicate that the mass of test particle does not influence the forms of temperature, entropy, and heat capacity but only changes their amplitudes.

The numerical methods indicate there are three situations corresponding to zero, one, and two diverging points of heat capacity respectively, which have been described in Figures 1, 2, and 3. Figure 1 shows a continuous phase and does not appear phase transition with . In Figure 2, there are one diverging point and two stable phases for with , phase 1 and phase 2, which individually represent a phase of large black hole (LBH) and a small black hole (SBH). In Figure 3, one can find there are three phases and two diverging points with . Phase 1 experiences a continuous process from a unstable phase to a stable phase ; phase 2 is a pure unstable phase with ; phase 3 is a stable phase with . It is easy to see phase 1 represents the phase of SBH and phase 3 represents the phase of LBH. However, there is a special unstable phase 2 between phase 1 and phase 3. This indicates when the system evolutes from phase 3 to phase 1, the system must experience a medium unstable state which could be explained as an exotic quark-gluon plasma with negative heat capacity [32, 33].