Research Article | Open Access

Akram Sadat Sefiedgar, "From the Schwarzschild Anti-de Sitter Black Hole to the Conformal Field Theory", *Advances in High Energy Physics*, vol. 2015, Article ID 841890, 7 pages, 2015. https://doi.org/10.1155/2015/841890

# From the Schwarzschild Anti-de Sitter Black Hole to the Conformal Field Theory

**Academic Editor:**Sally Seidel

#### Abstract

The emergence of the quantum gravitational effects in a very high energy regime necessitates some corrections to the thermodynamics of black holes. In this letter, we investigate a possible modification to the thermodynamics of Schwarzschild anti-de Sitter (SAdS) black holes due to rainbow gravity model. Using the correspondence between a ()-dimensional SAdS black hole and a conformal filed theory in -dimensional spacetime, one may find the corrections to the Cardy-Verlinde formula from the modified thermodynamics of the black hole. Furthermore, we show that the corrected Cardy-Verlinde formula can also be derived by redefining the Virasoro operator and the central charge.

#### 1. Introduction

Based on the great discovery of black hole Hawking radiation, it seems that there is a deep connection between three seemingly different branches of science: thermodynamics, gravity, and quantum mechanics in the black holes. In fact, Hawking radiation opens an important window to quantum gravity. Most of the promising candidates for quantum gravity expect the existence of a minimal observable length at the order of the Planck length [1–7]. Therefore, it is natural to take the Planck length as a universal constant [8]. On the other hand, length is obviously not an invariant under linear Lorenz boost. Therefore, the Lorentz symmetry at Planck scale may not be preserved. The goal of nonlinear special relativity or doubly special relativity (DSR) is to preserve the relativity principle and at the same time treat Planck length as an invariant [9]. Within nonlinear special relativity, the usual energy-momentum relation may be modified with corrections in the order of Planck length as where and are two general functions of energy with a constraint that they approach the unit for the energy scales much less than the Planck scale [10]. The modified dispersion relations may be responsible for threshold anomalies of ultra-high energy cosmic rays and gamma ray burst [11–17] and contribute corrections to the black hole thermodynamics [8]. Recently, nonlinear special relativity has been generalized to incorporate the effects of gravity, leading to the rainbow gravity model. In rainbow gravity, the metric of the background detected by any probe is not fixed but depends on the energy of the probe [18]. The rainbow gravity can be used to study the black holes. Of course, the thermodynamical properties of the black hole as well as the final fate of the black hole evaporation may be influenced by the effects of rainbow gravity.

On the other hand, one may relate the black hole thermodynamics with the properties of the conformal field theory (CFT) using the and correspondences. The Cardy-Verlinde (C-V) formula proposed by Verlinde relates the entropy of a certain conformal field theory to its total energy and its Casimir energy [19]. Using and correspondences, this formula holds exactly for different black holes. It means that one may find the quantum gravitational corrections to the C-V formula from the modified thermodynamics of black holes. Previously, the black holes had been considered to modify C-V formula from the generalized uncertainty principle [20, 21], space noncommutativity [22], and modified dispersion relations [23].

In this paper, we are going to take into account the corrections to the thermodynamics of a dimensional Schwarzschild anti-de Sitter black hole from the rainbow gravity. Knowing the corrections to the black hole thermodynamics, we can derive the corrections to the C-V formula. It is then shown that the modified C-V formula may also be derived by just redefining the Virasoro operator and the central charge.

#### 2. A Schwarzschild AdS Black Hole Thermodynamics within Rainbow Gravity

The metric of a dimensional Schwarzschild anti-de Sitter black hole in the rainbow gravity model can be written aswhich is the spherically symmetric solution of . Newton’s constant, , and the cosmological constant, , are energy dependent [24, 25]. The parameter is defined as and is the volume of a unit sphere. The position of the horizon, , can be derived by solving the equationSince investigating the black hole radiation and correction to entropy-area relation is an important subject in theoretical physics, we are going to study the black hole thermodynamics within rainbow gravity. On the black hole horizon, the surface gravity can be obtained byand it is possible to find the temperature from the surface gravity by [25].

For a dimensional Schwarzschild AdS black hole in the rainbow gravity, one can find the temperature aswhere is the modified temperature via rainbow gravity. It can be seen that the temperature of the modified black hole is different for probes with different energies. The temperature can be written aswhereis the black hole entropy without any corrections from rainbow gravity and is the temperature which is modified by taking into account the effects of and .

Now we are going to define an intrinsic temperature for large modified black holes by identifying probes with radiation particles in the vicinity of the horizon of the black hole. Using the radiation photons with average energy and to make the measurements, the temperature of the black hole can be identified with the energy of the photons emitting from the black hole as [25].

To find the black hole temperature, it is necessary to introduce the specific forms of the functions and . According to [8, 25, 26], we can writewhere is a positive quantity of order one which has been input to distinguish the correction terms arising from the rainbow gravity effects from the others. For , the energy-momentum relation reduces to its standard form in special relativity. By the definitions of and and plugging , (6) yields towhich can be solved to find the Schwarzschild AdS black hole temperature asFor large black holes with , the modified temperature reduces to the temperature of an ordinary Schwarzschild AdS black hole, . For small black holes with extremely high temperature, the temperature reaches its maximal value as . Correspondingly the radius of the black hole horizon is bounded from below by . The existence of a minimum radius leads to the possibility of the existence of the black hole remnant at the late moment of the evaporating process which can be a suitable candidate for dark matter.

By substituting into (10), the modified temperature can be written asAssuming that the correction terms are small, one may find by some manipulations thatFor large black holes, the first law of thermodynamics accompanying (10) yields towhich can be integrated to find as the modified entropy of a dimensional black hole within rainbow gravity. In (13), we have considered only the correction terms containing the first power of , without any loss of generality.

In the case of , the entropy of a dimensional Schwarzschild AdS black hole can be written aswhere . It is clear from (3) that can be obtained from . Furthermore, (12) can be expanded to find the temperature for a large dimensional Schwarzschild AdS black hole asIt is possible to write entropy in an alternative form as where is the standard entropy in the absence of rainbow gravity effects and implies the corrections to entropy via rainbow gravity. The temperature can also be written aswhere is the standard temperature in the absence of rainbow gravity effects and implies the corrections to the temperature via rainbow gravity.

In the case of , the entropy of a dimensional Schwarzschild AdS black hole can be written aswhere and the temperature isThe entropy can be written alternatively aswhereThe temperature can also be written aswhereThe quantities with prime refer to the modified ones in rainbow gravity while the quantities without prime do not imply any corrections from rainbow gravity. In the case of , it is clear from (3) that the radius of the horizon can be derived by .

As an important point, one may conclude that the predicted entropy within our formalism is smaller than that of the standard Bekenstein-Hawking entropy while the predicted temperature within our formalism is greater than that of the standard one. Furthermore, the entropy and the temperature of the black hole can be derived for any other dimensionality in the same manner. By continuing the procedure for higher dimensionality, one can deduce that the appearance of the logarithmic correction term in the entropy-area relation is restricted to even black hole dimensionality. In fact, if one tries to consider the higher order correction terms for different values of , the emergence of a logarithmic term in the entropy relation for even-dimensional black hole (odd ’s) will be certain. Using and correspondences, one can utilize the modified thermodynamics to have a more deep insight into CFT. Of course, insisting on the presence of a logarithmic term will put a constraint on the dimensionality of the black hole and its dual CFT. In particular, in the case of , the appearance of logarithmic correction term in the entropy-area relation is consistent with the results obtained in string theory and loop quantum gravity [27–30].

On the other hand, the modified dispersion relation is not confined only to rainbow gravity. In other words, MDR is a common feature to most of the quantum gravity candidates and, in particular, to the study of loop quantum gravity (LQG) and of models based on noncommutative geometry. In fact there has been strong interest in modifications to the energy-momentum dispersion relation [10, 31–37]. Therefore, the results obtained via MDR, which can be thought as the model independent results, seem to be of importance.

#### 3. Cardy-Verlinde Formula

The well-known Cardy formula gives the entropy of a 2-dimensional CFT as where is the product of energy and radius and the shift of is caused by the Casimir effect [38]. After making the appropriate identifications for and , the same Cardy formula is also valid for CFT in an arbitrary dimensional spacetime aswhich is called Cardy-Verlinde formula [19]. is the radius of the system, is the total energy, and is the Casimir energy defined asWe have computed the modified thermodynamics of a dimensional Schwarzschild anti-de Sitter black hole described by the C-V formula (27) from rainbow gravity.

Within rainbow gravity, by using equation one can substitute , , and into the equation to obtain the modified C-V formula asIt is necessary to point that we have replaced by from [23]. Assuming that the correction terms are small, we have ignored their product and used Taylor expansion to derive (31). Now we can represent the entropy of the conformal field theory which lives in a -dimensional spacetime by and it can be derived using the thermodynamical properties of a dimensional black hole.

In the case , the modified C-V formula can be written aswhere , , , and can be substituted from (17) and (19) in terms of the related . The modified entropy of the conformal field theory which lives in a -dimensional spacetime has been represented by while is the entropy of the CFT in the absence of the rainbow gravity effects.

In the case , the modified C-V formula will bewhere , , , and can be substituted from (23) and (25) in terms of the related . The modified entropy of the conformal field theory which lives in a -dimensional spacetime is represented by while is the entropy of the CFT in the absence of the rainbow gravity effects.

In 2-dimensional conformal field theory, when the conformal weight of the ground state is zero, the valid form of C-V formula iswhere is the central charge and is the Virasoro operator [21, 39]. If we use in (27), where is the Casimir entropy, and drop in analogy with (34), we obtain the generalization to (34) for a dimensional CFT [21, 39] aswhereNow (35) can be applied to a Schwarzschild anti-de Sitter black hole. In fact, The C-V formula is the outcome of a striking resemblance between the thermodynamics of CFTs with asymptotically AdS duals and CFTs in two dimensions [21, 39]. Therefore, it is possible to take into account the corrections to C-V formula by just redefining the Virasoro operator and the central charge, the quantities entering the C-V formula. Using , the Virasoro operator can be modified toThe modified central charge can be written aswhere the second orders of the corrections terms have been neglected and the relation has been applied.

In the case of ,where

In the case of ,where Using (35), the modified Virasoro operator and the modified central charge can be applied to find the corrections to C-V formula for a dimensional CFT. It is clear that one can find the corrections to the C-V formula for any other CFT dimensionality in the same manner.

#### 4. Conclusions

We have computed the thermodynamical properties of a dimensional Schwarzschild anti-de Sitter black hole within rainbow gravity. The corrected entropy, temperature, and energy of the black hole have been used to modify the C-V formula. Since the C-V formula refers to the entropy of a dual conformal field theory living on the dimensional boundary space, the modified entropy of the CFT has been obtained. We also stressed the point that the C-V formula is the outcome of a resemblance between the thermodynamics of CFTs with asymptotically AdS duals and CFTs in two dimensions. Then we have derived the corrections to the Virasoro operator and the central charge, the quantities which are entering the C-V formula. We have shown the possibility of taking into account the rainbow gravity corrections to the C-V formula by just redefining the Virasoro operator and the central charge.

#### Conflict of Interests

The author declares that there is no conflict of interests regarding the publication of this paper.

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#### Copyright

Copyright © 2015 Akram Sadat Sefiedgar. 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}.