Quantum Tunneling Radiation from Loop Quantum Black Holes and the Information Loss Paradox

Abstract

In this work, we present some results relating to the issue of the Loop Quantum Black Holes (LQBH) thermodynamics by the use of the tunneling radiation formalism. The information loss paradox is also discussed in this context, and we have considered the influence of back reaction effects.

1. Introduction

Starting from the Hawking demonstration, made in the 1970s, which shows that black holes can radiate thermally [1], some work has been undertaken in order to understand the black hole evaporation phenomenon. In this sense, several methods have been developed in order to calculate the temperature and entropy of black holes [2,3,4,5]. However, some questions about the black hole evaporation process remain open until now, such as the information loss paradox [6,7] and the issue about the origin of black hole entropy [8].

Among the methods that have been developed in order to understand black hole evaporation, more recently, a semiclassical method has been constructed upon the interpretation of Hawking radiation as a tunneling process across the black hole horizon [9,10,11]. The basic idea is that the Hawking flux, observed at infinity, has its origin in positive energy particles created just inside the horizon which could tunnel through it quantum mechanically. The tunneling approach is especially interesting in order to calculate black hole temperature since it provides a dynamic model for the black hole emission process. In this way, the tunneling approach turns out to be very useful when one wishes to incorporate back-reaction effects in order to describe black hole evaporation. In addition, even though calculations in the tunneling formalism are straightforward and relatively simple, they are robust in the sense that they can be applied to a wide variety of spacetimes [12,13,14,15,16,17,18,19,20,21,22,23,24,25].

Tunneling formalism has also contributed to the discussion of the black hole information loss paradox, even at the semiclassical level. In this way, Parikh [10] demonstrated, at first, that a nonthermal spectrum could be calculated when one interprets the black hole emission process as a tunneling phenomena. However, no information recovery was obtained from the Parikh analysis. Such treatment was used also by Arzano et al. [26] where quantum gravity effects was considered. However, Zhang et al. [27] have demonstrated that the Parikh argument needed to be rectified. In this way, by the use of a statistical argument, Zhang et al. have shown that in the view of the tunneling approach, some information could be recovered by black holes during their evaporation process.

On the other hand, in the framework of black hole evaporation, it is expected that quantum gravity effects must have a crucial role, especially in the last stages of black hole evaporation. In this way, additional investigations taking into account quantum gravity contributions to the black hole emission process have been done by considering noncommutative geometry, Generalized Uncertainty Principle (GUP), as well as Loop Quantum Gravity (LQG) and string theory scenarios [28,29,30,31,32,33,34,35,36,37], where the information loss issue has also been considered.

In this work, at first, we shall revisit the results of [38] where the Hamilton-Jacobi version of the tunneling formalism can be used to investigate how quantum gravity effects could have an influence in the emission process by means of a black hole. In order to do this, we shall investigate the thermodynamic properties of Loop Quantum Black Holes [39,40], which correspond to a quantum corrected black hole solution that appears in the context of LQG. The temperature and entropy of this kind of black hole are calculated by the use of the tunneling method. These first results presented in [38] replicate those found in the references [40,41,42], where other methods have been used. In this way, it can be demonstrated that the quantum tunneling formalism can be successfully applied to address the thermodynamics of LQBHs, opening a path for a whole range of applications. Among the possible applications, in the present paper, we shall investigate the possibility of information recovery through the calculation of the statistical correlations between consecutive modes emitted during the LQBH evaporation. In this case, the results of [38], which were based on the Parikh approach, have been improved by the use of the treatment introduced by Zhang et al. In order to perform the two last tasks, back reactions effects will be taken into account, since it is supposed that such effects could give us a mechanism for information recovery at the last stages of black hole evaporation.

This paper is organized as follows. In Section 2, we review the main features of the LQBHs scenario. In Section 3, we review the use of the tunneling formalism to calculate the temperature and entropy of LQBHs. In Section 4, we shall see how back reactions effects can be included. In Section 5, we shall address the information loss problem in the LQBH scenario by the use of the tunneling formalism. The last section is devoted to remarks and conclusions.

2. Loop Quantum Black Holes

Efforts in order to find out black holes solutions in the context of LQG have been made by several authors [43,44,45,46,47,48,49,50,51,52,53,54,55,56]. In this work, we shall investigate the thermodynamics of a particular solution called the self-dual solution which was obtained by the use of loop quantum cosmology quantization techniques to the Schwarzschild scenario [39].

The self-dual black hole solution is obtained in the semiclassical limit of LQG. Even though the semiclassical limit of the full theory of LQG is not completely understood yet, the situation is quite different in the case of symmetry-reduced models where the semiclassical limit can be performed in a trustable form [57].

In this way, the self-dual black hole scenario is obtained by the reduction from the full LQG theory to the minisuperspace model by spherical symmetric reduction of the Hamiltonian constraint [39]. The semiclassical approximation of the Hamiltonian is then performed and a quantum gravitationally corrected Schwarzschild solution, described by the following metric, is obtained

$$d{s}^2=-G\left(r\right)c^{2}d{t}^2+F{\left(r\right)}^{-1}d{r}^2+H\left(r\right)d{\mathsf{\Omega }}^2,$$

(1)

with

$$d{\mathsf{\Omega }}^2=d{\theta }^2+{sin}^2\theta d{\varphi }^2.$$

(2)

In the Equation (1), the metric functions are given by

$$G\left(r\right)=\frac{(r-r_{+})(r-r_{-})(r-r_{*})}{r^4+a_0^2},$$

(3)

$$F\left(r\right)=\frac{(r-r_{+})(r-r_{-})r^4}{{(r+r_{*})}^2(r^4+a_0^2)},$$

(4)

and

$$H\left(r\right)=r^2+\frac{a_0^2}{r^2},$$

(5)

where

$$\begin{array}{c}\hfill r_{+}=\frac{2Gm}{c^2};r_{-}=\frac{2Gm}{c^2}{P}^2.\end{array}$$

In the loop black hole scenario, we have the presence of two horizons—an event horizon and a Cauchy horizon. Moreover, $r_{*}$ is defined as

$$\begin{array}{cc}\hfill r_{*}=& \sqrt{r_{+}{r}_{-}}=\frac{2Gm}{c^2}P,\end{array}$$

(6)

where P is the polymeric function [39].

Moreover, $a_0=\frac{A_{\min }}{8\pi }$, where $A_{\min }$ represents the minimal value of area in Loop Quantum Gravity, and the mass parameter m is related with the ADM mass M by

$$m=M(1+P).$$

(7)

In this way, the LQBH scenario consist in a semiclassical scenario which differs from the classical Schwarzschild solution by the presence of quantum corrections in terms of the polymeric function P and the LQG minimal area. The classical Schwazschild scenario is restored when one takes the limit where $a_0\to 0$ and $P\to 0$. The complete treatment regarding the way that the LQBH scenario is obtained from LQC is archived in [39].

In order to discuss the properties of LQBH solution, let us write the Kretschmann invariant for this solution which, for $r\approx 0$, is given by

$$K=R_{\mu \nu \alpha \beta }{R}^{\mu \nu \alpha \beta }=\frac{3145728{\pi }^4{r}^6}{a_0^4{\gamma }^8{\delta }^8{m}^2}.$$

(8)

Consequently, in a different way from the classical Schwarzschild solution, the LQBH Kretschmann invariant does not diverge when $r\to 0$. This fact indicates that the resolution of the black hole singularity at $r=0$. In fact, in the LQBH scenario, the black hole singularity is replaced by another asymptotic flat region, as can be seen in the LQBH Carter-Penrose diagram depicted in Figure 1.

The LQBH spacetime possess yet another interesting property, that of self-duality. This property is given by a symmetry present in the metric (1). In this way, the LQBH metric is invariant by the transformations $\tilde{r}=a_0/r$ and $\tilde{t}=t{r}_{*}^2/a_0$, with ${\tilde{r}}_{\pm }=a_0/r_{\mp }$. Such transformations connect the description of an outside to an inside observer, where the first sees a black hole with mass m described by the metric (1) while the inside observer sees a black hole with mass $1/m$ described by the dual metric. From the self-duality property, in a different way from the classical Schwarzschild solution, the LQBH scenario allows black holes to have a mass smaller than the Planck mass [39].

Another interesting feature of the LQBH scenario comes from the fact that, in the metric (1), r is only asymptotically the radial coordinate. This is because $g_{\theta \theta }$ is not given by $r^2$ but by $H\left(r\right)$. In this way, the physical radial coordinate, defined in order to measure the proper circumferential distance, is given by

$$R=\sqrt{r^2+\frac{a_0^2}{r^2}}.$$

(9)

The Equation (9) reveals vital aspects of the LQBH’s internal structure. From this expression, we obtain that, as r decreases from ∞ to 0, R initially decreases from ∞ to $\sqrt{2a_0}$, at $r=\sqrt{a_0}$, so it will increase once more to ∞. In this way, we have that, at the limit of $r\to 0$, we shall have another asymptotically flat Schwarzschild region rather than a singularity as has been depicted in the Carter-Penrose diagram (1). Such a new region corresponds to a wormhole whose dimensions are the order of the Planck length. The wormhole throat is described by the Kantowski-Sachs spacetime [58].

The thermodynamical properties of LQBH can be obtained from the metric (1). In fact, the Bekenstein-Hawking temperature $T_{BH}$ is related with the surface gravity $\kappa$ which is given by

$${\kappa }^2=-g^{\mu \nu }{g}_{\rho \sigma }{\nabla }_{\mu }{\chi }^{\rho }{\nabla }_{\nu }{\chi }^{\sigma }=-\frac{1}{2}{g}^{\mu \nu }{g}_{\rho \sigma }{\mathsf{\Gamma }}_{\mu 0}^{\rho }{\mathsf{\Gamma }}_{\nu 0}^{\sigma },$$

(10)

where, in the expression above, ${\chi }^{\mu }=(1,0,0,0)$ is identified as a timelike Killing vector and ${\mathsf{\Gamma }}_{\sigma \rho }^{\mu }$ are the connections coefficients.

In this way, from the metric (1), we obtain

$$T_H=\frac{\hslash }{2\pi c}\kappa =\frac{\hslash c^3}{4\pi G{k}_B}\frac{{\left(2m\right)}^3(1-P^2)}{[{\left(2m\right)}^4+a_0^2]}.$$

(11)

As we can observe, the temperature above agrees with the classical Hawking temperature in the large mass limit. On the other hand, it goes to zero for $m\to 0$.

The entropy of LQBH is obtained from the usual thermodynamical relation $S_{BH}=\int c^{2}dm/T\left(m\right)$, which gives us

$$S=\frac{4\pi k_B{c}^3}{\hslash G}\frac{{(1+P)}^2}{(1-P^2)}\left[\frac{16m^4-a_0^2}{16m^2}\right].$$

(12)

Further investigations about LQBH have been performed in order to calculate the gravitational wave spectrum and the gravitational lensing by this kind of black hole [59,60]. Moreover, the entropy-area relation that appears in the context of LQBH has been used in order to derive, based on a thermodynamical argument, quantum corrected bounce-type Friedmann equations [61], in agreement with the standard loop quantum cosmology [62].

As we can see, the LQBH metric brings quantum gravity corrections, expressed in terms of LQC parameters like P and $a_0$, to the black hole thermodynamical properties like temperature and entropy. Such corrections could induce modifications in the way how the black hole evaporates. In the following, we shall use the quantum tunneling formalism in order to address the thermodynamical properties of LQBHs. The information loss problem will also be addressed in this context.

3. Quantum Tunneling Radiation from Loop Quantum Black Holes

In 2000, Parikh and Wilczec [9], following previous discussions by Krauss and Wilczec [63,64,65], developed the first tunneling method in order to describe the black hole evaporation process, named the null geodesic method. Subsequently, in 2005, Angheben et al. [16] presented an alternative description to the black hole tunneling process based on a Hamiltonian-Jacobi ansatz, consisting of an extension of the complex path analysis developed by Padmanabham et al. [25,66,67,68].

By the use of the Hamilton-Jacobi method introduced by Angheben et al., the thermodynamical properties of LQBHs have been investigated by Silva and Brito [38], where the inclusion of back reaction effects and the information loss problem have been addressed. However, the discussion about the information loss problem undertaken in [38] has been based on an approach introduced by Parikh [10] which has been rectified by Zhang et al. [27].

In this way, we shall at first review the results of [38] related to the calculation of LQBH temperature and entropy and the inclusion of back reaction effects. In the Section 5, we shall improve the results of [38] related to the issue of information recovery, by the use of the approach introduced by Zhang et al. Regarding this point it is necessary to emphasize that the tunneling method, which works in the semiclassical level, will be applied here to a semiclassical black hole solution that appears in the context of LQG. In this way, even though the spacetime in LQG is discrete, the black hole geometry we consider here is an effective geometry that is obtained by taking the semiclassical limit of a symmetry reduced model of LQG [39].

In this way, we have that, near the event horizon, one could reduce the description of the particle emission by a black hole to a 2-dimensional theory [69,70], where the metric corresponds to the $(t-r)$ sector of the original metric since its angular part is red-shifted away in this limit. Therefore, the near-horizon metric becomes:

$$d{s}^2=-G\left(r\right)c^{2}d{t}^2+F{\left(r\right)}^{-1}d{r}^2.$$

(13)

In addition, in the near-horizon limit, the effective potential vanishes and there are no grey-body factors.

Now, let us consider the Klein-Gordon equations

$${\hslash }^2{g}^{\mu \nu }{\nabla }_{\mu }{\nabla }_{\nu }\varphi -m^2{c}^2\varphi =0,$$

(14)

which, by the application of the metric (13) give us

$$-\frac{1}{c^2}{\partial }_t^2\varphi +\mathsf{\Lambda }{\partial }_r^2\varphi +\frac{1}{2}{\mathsf{\Lambda }}^{\prime }{\partial }_r\varphi -\frac{m^2{c}^2}{{\hslash }^2}G\left(r\right)\varphi =0,$$

(15)

where $\mathsf{\Lambda }=F\left(r\right)G\left(r\right)$.

At this point, we shall take the standard WKB ansatz:

$$\varphi (r,t)=e^{-\frac{i}{\hslash }I(r,t)}.$$

(16)

Such WKB approximation is justified by the fact that, when the outgoing wave is traced back towards the horizon, its wavelength, as measured by a local fiducial observer, is ever-increasingly blue shifted and the point particle interpretation can be allowed [9].

In this way, by the use of the WKB ansatz (16), one obtains the relativistic Hamilton-Jacobi equation, in the limit of $\hslash \to 0$:

$$\frac{1}{c^2}{\left({\partial }_{t}I\right)}^2-\mathsf{\Lambda }{\left({\partial }_{r}I\right)}^2-m^2{c}^{2}G\left(r\right)=0.$$

(17)

We shall seek a solution in the form:

$$I(r,t)=-\omega t+W\left(r\right).$$

(18)

in a way that we obtain

$$W=\int \frac{dr}{\mathsf{\Xi }}\sqrt{\frac{1}{c^2}{\omega }^2-m^2{c}^{2}G},$$

(19)

where $\mathsf{\Xi }={\mathsf{\Lambda }}^{1/2}$.

In this point, we shall adopt the proper spatial distance

$$d\sigma =\frac{d{r}^2}{\mathsf{\Xi }\left(r\right)},$$

(20)

where, by taking the near horizon approximation, we obtain

$$\mathsf{\Xi }\left(r\right)={\mathsf{\Xi }}^{\prime }\left(r_H\right)(r-r_H)+\dots .$$

(21)

In this way, we find that

$$\sigma =2\frac{\sqrt{r-r_H}}{{\mathsf{\Xi }}^{\prime }\left(r_H\right)},$$

(22)

where $0<\sigma <\infty$.

In terms of the proper spatial distance, we obtain for the spatial part of the action I

$$\begin{array}{ccc}\hfill W& =& \frac{2}{{\mathsf{\Xi }}^{\prime }\left(r_H\right)}\int \frac{d\sigma }{\sigma }\sqrt{\frac{1}{c^2}{\omega }^2-\frac{{\sigma }^2}{4}{m}^2{c}^2{G}^{\prime }\left(r_H\right){\mathsf{\Xi }}^{\prime }\left(r_H\right)}\hfill \\ & =& \frac{2\pi i\omega }{{\mathsf{\Xi }}^{\prime }\left(r_H\right)c}+\mathrm{real}\mathrm{contribution}.\hfill \end{array}$$

(23)

In this way, the tunneling probability of the emission of a particle with energy $\omega$ will be given by

$$\mathsf{\Gamma }\backsimeq Exp[-\frac{2}{\hslash }ImI]=Exp\left\{-\frac{\pi G}{c^3\hslash }\frac{[{\left(2m\right)}^4+a_0^2]}{m^3(1-P^2)}\omega \right\}.$$

(24)

Now, assuming a Boltzmann form, $\mathsf{\Gamma }\sim e^{-\beta \omega }$, for the emission probability above, where $\beta$ is the inverse temperature $\beta =1/k_B{T}_H$, we obtain the LQBH temperature as:

$$T_H=\frac{\omega }{ImI}=\frac{\hslash c^3}{4\pi G{k}_B}\frac{{\left(2m\right)}^3(1-P^2)}{[{\left(2m\right)}^4+a_0^2]},$$

(25)

which coincides with the former Expression (11) found out in the references [40,41,42].

From the expression for LQBH temperature, one obtains for the entropy:

$$S=\frac{4\pi k_B{c}^3}{\hslash G}\frac{{(1+P)}^2}{(1-P^2)}\left[\frac{16m^4-a_0^2}{16m^2}\right].$$

(26)

From the results above, we have that the tunneling formalism is straightforward in order to calculate the LQBH thermodynamical properties. Such results pave the way for many applications, some of which we shall address in the following sections.

4. Back Reaction Effects

Based on the results obtained in the last section, which demonstrated that the tunneling approach is appropriate to calculate the thermodynamical properties of LQBHs, following the results of [38], in this section we shall discuss how back reaction effects can be introduced in the description of its evaporation process. By taking into account such self-gravitational effects, in this way, one can refine the description of LQBH thermodynamics, mainly in the quantum gravitational regime. This is because back reaction effects must be taken into account in the late stages of black hole evaporation, where the usual framework for the emission process will loose its validity [9,10,11,23,25,64,66,67,71,72,73,74,75,76,77].

In this way, in the Hamilton-Jacobi formalism, back reaction effects can be introduced when one takes the action I to be given by the following relation [78]

$$I=-\frac{i}{2}\frac{\hslash }{k_B}[S(M-\omega )-S\left(M\right)],$$

(27)

where M is identified as the black hole ADM mass.

In the case of LQBHs, we shall take, for practical purposes, the changing in the mass parameter m related with the black hole ADM mass through the Equation (7). Therefore, we shall consider that a reduction in the black hole ADM mass will correspond to a reduction of $\epsilon =\omega {(1+P)}^2$ in the mass parameter m.

Let us consider the following relation:

$$\begin{array}{ccc}\hfill I& =& -\frac{i}{2}\frac{\hslash }{k_B}[S(m-\epsilon )-S\left(m\right)]\hfill \\ & =& -\frac{4\pi c^3}{G}\frac{i{(1+P)}^2}{(1-P^2)}\epsilon (\epsilon -2m)\left[1-\frac{a_0^2}{16m^2{(m-\epsilon )}^2}\right].\hfill \end{array}$$

Consequently, we shall have, for the probability of the black hole emit a quanta with energy $ϵ$, when back-reaction effects are taken into account:

$$\begin{array}{ccc}\hfill \mathsf{\Gamma }\left(\epsilon \right)& =& Exp\left\{\frac{4\pi c^3}{G\hslash }\frac{{(1+P)}^2}{(1-P^2)}\epsilon (\epsilon -2m)\left[1-\frac{a_0^2}{16m^2{(m-\epsilon )}^2}\right]\right\}.\hfill \end{array}$$

(28)

In the next section, we shall apply these results in order to investigate the possibility to have some correlation between the quanta emitted by a LQBH due to quantum gravity corrections present in this scenario.

5. Information Recovery from LQBHs

In order to solve the black hole information loss paradox, many proposals have been made [79,80,81,82,83,84,85] (For a recent review, see [86]). Among these proposals, we have the idea that information lost behind the black hole event horizon could re-emerge via Hawking radiation by some process. The late stages of black hole evaporation consist of an interesting scenario in order to have some mechanism of information recovering through Hawking radiation. This is because, as has been emphasized in the last section, the usual description for the emission process will loose its validity at these stages, and gravitational back-reaction effects must be taken into account [9,10,11,23,25,64,66,67,71,72,73,74,75,76,77].

In order to investigate if some information can be recovered during the black hole evaporation, one can investigate if there exist statistical correlations between the Hawking modes emitted. This method was applied, at first by Parikh [10] and Arzano et al. [26] and consists of considering two emissions with energies ${\epsilon }_1$ and ${\epsilon }_2$, or one emission with energy ${\epsilon }_1+{\epsilon }_2$. The statistical correlation between two Hawking modes emitted by a black hole can be measured by the function:

$$C({\epsilon }_1+{\epsilon }_2;{\epsilon }_1,{\epsilon }_2)=ln\left[\mathsf{\Gamma }({\epsilon }_1+{\epsilon }_2)\right]-ln\left[\mathsf{\Gamma }\left({\epsilon }_1\right)\mathsf{\Gamma }\left({\epsilon }_2\right)\right].$$

(29)

It has been initially demonstrated by Parikh and Wilczek [9] that non-thermal corrections to the black hole radiation spectrum can be obtained when one takes into account back reaction effects. However, Parikh at first demonstrated that, in the classical treatment by the aforecited authors, no statistical correlation between the quanta emitted by a black hole has been found [10]. Such treatment was later followed up by Arzano et al. [26]. On the other hand, based upon standard statistical methods, by distinguishing statistical dependence or independence of sequential emissions, Zhang et al. demonstrated that a statistical correlation can be established between the quanta emitted by a black hole [27]. In this way, by the use of the approach introduced by Zhang et al., we shall refine the results of [38] which was constructed upon the Parikh and Wilczek argument.

In order to do this, we have that the probability distribution for the simultaneous emission of two modes with energies ${\epsilon }_1$ and ${\epsilon }_2$ is given by

$$\begin{array}{ccc}\hfill \mathsf{\Gamma }({\epsilon }_1,{\epsilon }_2)& =& \mathsf{\Gamma }({\epsilon }_1+{\epsilon }_2)\hfill \\ & =& Exp\left\{\frac{4\pi c^3}{G\hslash }\frac{{(1+P)}^2}{(1-P^2)}({\epsilon }_1+{\epsilon }_2)[({\epsilon }_1+{\epsilon }_2)-2m]\left[1-\frac{a_0^2}{16m^2{(m-({\epsilon }_1+{\epsilon }_2))}^2}\right]\right\},\hfill \end{array}$$

(30)

which is subject to a normalization factor $\mathsf{\Lambda }$ which is fixed by

$$\mathsf{\Lambda }{\int }_0^M\mathsf{\Gamma }\left(\epsilon \right)d\epsilon =1.$$

(31)

On the other hand, the probability distributions for two independent emissions ${\epsilon }_1$ and ${\epsilon }_2$ are given by

$$\mathsf{\Gamma }\left({\epsilon }_1\right)=\mathsf{\Lambda }{\int }_0^{M-{\epsilon }_1}\mathsf{\Gamma }({\epsilon }_1,{\epsilon }_2)d{\epsilon }_2=Exp\left\{\frac{4\pi c^3}{G\hslash }\frac{{(1+P)}^2}{(1-P^2)}{\epsilon }_1({\epsilon }_1-2m)\left[1-\frac{a_0^2}{16m^2{(m-{\epsilon }_1)}^2}\right]\right\}$$

(32)

and

$$\mathsf{\Gamma }\left({\epsilon }_2\right)=\mathsf{\Lambda }{\int }_0^{M-{\epsilon }_2}\mathsf{\Gamma }({\epsilon }_1,{\epsilon }_2)d{\epsilon }_1=Exp\left\{\frac{4\pi c^3}{G\hslash }\frac{{(1+P)}^2}{(1-P^2)}{\epsilon }_2({\epsilon }_2-2m)\left[1-\frac{a_0^2}{16m^2{(m-{\epsilon }_2)}^2}\right]\right\}.$$

(33)

Therefore, considering the quantum gravity corrections from LQBHs, using the Equation (28), the correlation function between two consecutive modes with energies ${\epsilon }_1$ and ${\epsilon }_2$ will be given by:

$$\begin{array}{cc}\hfill C({\epsilon }_1+{\epsilon }_2;{\epsilon }_1,{\epsilon }_2)=& \frac{8\pi {(1+P)}^2}{{(1-P)}^2}\frac{c^3}{G\hslash }{\epsilon }_1{\epsilon }_2-\frac{\pi a_0^2{(1+P)}^2}{4(1-P^2)m^2}\frac{G}{c^3\hslash }\{\frac{({\epsilon }_1+{\epsilon }_2)({\epsilon }_1+{\epsilon }_2-2m)}{{(m-{\epsilon }_1-{\epsilon }_2)}^2}\hfill \\ \hfill -& \left[\frac{{\epsilon }_1({\epsilon }_1-2m)}{{(m-{\epsilon }_1)}^2}+\frac{{\epsilon }_2({\epsilon }_2-2m)}{{(m-{\epsilon }_2)}^2}\right]\},\hfill \end{array}$$

(34)

where the semiclassical term found out by [27] appears, unless the polymeric function, with a quantum gravity correction which comes from the LQBH metric. In the Figure 2, the correlation functions for a classical and for a LQBH are compared.

As we can observe, the quantum gravity contributions to the black hole evaporation process from the LQBH can, when compered with a classical black hole, relieve in a more substantial way the information loss problem. Such effects become more evident when the black hole approaches the Planck scale, in the final stages of the emission process, where both back-reaction and quantum gravity effects become more important.

6. Conclusions and Remarks

In this work, at first, we have revisited the results of [33] relating to the investigation of the LQBH thermodynamics by the use of the Hamilton-Jacobi version of the tunneling formalism. We have shown that the results obtained in the references [40,41,42] for the LQBH temperature and entropy can be reproduced by the use of the tunneling method, in a way that such a method can be, in fact, reliably applied in order to address LQBH thermodynamics. We have also presented the results related with the inclusion of back reaction effects in the description of the LQBH evaporation process. Such effects are important in order to understand the thermodynamical dynamics of black holes during the late stages of their evaporation, where quantum gravity becomes important and the usual thermodynamical approach to such phenomena fails.

Finally, we have addressed the possibility of recovery of some information during the LQBH evaporation process, mainly during the its late stages. The results of the present work have revealed that the modes emitted by a LQBH are related by a non-thermal correlation function with a quantum gravity contribution. Consequently, some information can be recovered during the LQBH evaporation process. The results presented in this paper, related with correlation functions, calculated upon the argument by Zhang et al. [27], improve the results of [33], based on the Parikh argument [10].