# Self-Regular Black Holes Quantized by means of an Analogue to Hydrogen Atoms

Authors: Chang Liu; Yan-Gang Miao; Yu-Mei Wu; Yu-Hao Zhang
Journal: Advances in High Energy Physics
 (2016)

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## Abstract

We suggest a quantum black hole model that is based on an analogue to hydrogen atoms. A self-regular Schwarzschild-AdS black hole is investigated, where the mass density of the extreme black hole is given by the probability density of the ground state of hydrogen atoms and the mass densities of nonextreme black holes are given by the probability densities of excited states with no angular momenta. Such an analogue is inclined to adopt quantization of black hole horizons. In this way, the total mass of black holes is quantized. Furthermore, the quantum hoop conjecture and the Correspondence Principle are discussed.


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## Body

## 1. Introduction

It has been desirable that a nonperturbative quantum gravity theory should have no ultraviolet (UV) divergences [1–4]. To be consistent with this feature, the self-complete gravity theory [5, 6] has been put forward to give a short distance cutoff that naturally avoids the UV divergence. Normally, the probe energy must be higher and higher when the exploration of microscope gets deeper and deeper. However, the production of micro black holes provides a possible way to circumvent such an endless procedure. The UV self-completeness renders an intriguing property that micro black holes would be produced if elementary particle collisions with the Planckian energy scale could satisfy the so-calledquantum hoop conjecture [7]. When the energy goes higher, one cannot probe shorter distances but produce greater black holes with bigger horizons, where such objects are called classicalons [5, 6, 8–10]. This means that the horizon of micro black holes gives a threshold or a natural minimal length that might be probed experimentally. On the other hand, if the minimal length implies the Planck length, the corresponding energy scale is far from being reached by the present and even foreseeing colliders. Nonetheless, if the effect of large extra dimensions could be considered, the micro black holes with the TeV scale would probably be produced at the LHC or its next generation in a nonfar future. In the recent decade or so, there has been much progress on this issue, both in theory [11–27] and in experiment [28–32].The idea of the self-completeness mentioned above has been realized by Nicolini et al. [33] when the noncommutative geometry [34] is introduced into the ordinary Schwarzschild black hole. It is assumed that the noncommutativity of spacetime would be an intrinsic rather than a super-imposed property of manifold, so that one should modify the distribution of matter and consequently the modified distribution of matter naturally reflects the basic characteristic of noncommutativity in manifold [35]. That is to say, energy-momentum tensors are modified in terms of smeared matter distributions in the right hand side of Einstein’s field equations, while no changes are made in the left hand side. By inserting the condition of energy conservation, ∇ μ T μ ν = 0, into a Schwarzschild-like solution, g 00 g r r = - 1, a mass-smeared spherically symmetric black hole solution of the modified Einstein equations with a Gaussian mass density [33] can be obtained. The self-regular solution has no singularity at the origin and it naturally contains a minimal length that originates from the horizon of an extreme black hole. If the point-like mass distribution with the Dirac δ-function density is taken, one obtains the ordinary Schwarzschild-AdS solution by solving the modified Einstein equations. For more details about this self-regular model of black holes, see [36–39].Based on such a modification of mass distribution mentioned above, a new self-regular quantum black hole proposal [40] has been put forward by making an analogy between a self-regular black hole and a harmonic oscillator. As the Gaussian mass density is proportional to the probability density of the ground state of a harmonic oscillator, the self-regular Schwarzschild black hole is regarded as a quantum harmonic oscillator. As a result, the total mass of the extreme self-regular Schwarzschild black hole is associated with the zero-point energy of a harmonic oscillator. In addition, the specific mass densities (Such mass densities are not set to be the probability densities of the excited states of a harmonic oscillator in order to avoid the appearance of multihorizon geometries for the nonextreme black holes, which leads to the proposal being Bohr-like quantization, as explained in [40].) with no multihorizon geometries are chosen for nonextreme black holes. As it is assumed that the nonextreme black holes correspond to the excited states of a harmonic oscillator, the total masses of nonextreme black holes are thus associated with the energy eigenvalues of the excited states of a harmonic oscillator. Moreover, the quantum hoop conjecture and Correspondence Principle related to the analogy with a harmonic oscillator are found to be satisfied. The proposal briefly summarized above is named [40] as the Bohr-like quantization of the Schwarzschild black hole.Inspired by the interesting Bohr-like quantization [40], we propose in the present paper the so-called Schrödinger-like quantization for the self-regular Schwarzschild-AdS black hole. The meaning relies on our choice of black hole mass densities that depends on solutions of the Schrödinger equation not only for an extreme black hole but also for a nonextreme one. Although such a choice for a nonextreme black hole leads normally to the appearance of multihorizon geometries, it is well known that an extreme black hole, sometimes also named as a remnant of black holes at the final stage of the Hawking radiation, is quite different from a nonextreme one and therefore it seems to be far-fetched to require both of them monohorizontally. The merit of our choice is that we provide a unified source of black hole mass densities for both the extreme and nonextreme cases, which makes our proposal succincter. Besides the formulations of mass densities, the other indispensable ingredient in the Bohr-like or our proposal is a special model of quantum mechanics that will be used to make an analogy with the black hole we are trying to quantize. Instead of a harmonic oscillator associated with the Bohr-like quantization [40], we take a hydrogen atom as our specific model. The reason of our choice comes from the recent works by Corda [41–44] and Bekenstein [45], where the radiation spectrum of black holes is interpreted (We would like to point out that these works just established the analogy between the Hawking radiation spectra and the energy levels of a hydrogen atom, i.e., the quantization of the radiation spectra, in a semiclassical approach. However, the quantization of the black hole itself was not touched, which leaves the task to the present paper.) to be similar to that of a hydrogen atom. That is, these works imply that there is a deep internal relationship between black holes and hydrogen atoms. Consequently, based on the Bohr-like quantization and the recent works by Corda and Bekenstein, we propose our scenario for quantization of the self-regular Schwarzschild-AdS black hole: the first step is to make the analogy between this black hole and the hydrogen atom, and then the second step is to choose the probability densities of states of hydrogen atoms to be the mass densities not only for an extreme black hole but also for a nonextreme one.The arrangement of this paper is as follows. In Section2, we start from the metric of the self-regular Schwarzschild-AdS black hole, where the original total mass of a black hole has been replaced by a mass distribution. In this way, the noncommutativity of spacetime is introduced [33] into the Schwarzschild-AdS black hole and thus the curvature singularity at the origin is canceled. Further, the probability densities of the ground state and excited states of hydrogen atoms are chosen to be the mass densities of the extreme and nonextreme self-regular Schwarzschild-AdS black holes, where the ground state of hydrogen atoms corresponds to the extreme black hole and the excited states correspond to the nonextreme ones, which realizes the analogy between the self-regular Schwarzschild-AdS black hole and the hydrogen atom. Then, we analyze the mass quantization of the self-regular Schwarzschild-AdS black hole in Section 3 through quantization of horizons. Such an analysis depends on the mean radius of hydrogen atoms, which is consistent with our specific analogy. Moreover, the quantum hoop conjecture and the Correspondence Principle related to such an analogy are discussed. Finally, Section 4 is devoted to a brief conclusion.


## 2. Analogy between Self-Regular Black Holes and Hydrogen Atoms

The metric of the static and spherically symmetric self-regular Schwarzschild-AdS black hole, where the noncommutativity of spacetime has been considered, takes the form(1) d s 2 = - 1 - 2 M r r + r 2 b 2 d t 2 + 1 - 2 M r r + r 2 b 2 - 1 d r 2 + r 2 d θ 2 + sin 2 ⁡ θ d ϕ 2 ,where the parameter b is the radius of the AdS background spacetime. This metric is the so-called self-regular or noncommutative geometry inspired formulation of the Schwarzschild-AdS black hole with no metric and curvature singularities at the origin [33, 36–39]. The characteristic of this kind of black holes is that the mass distribution,(2) M r = ∫ 0 r ρ r 4 π r 2 d r ,replaces the total mass, M = ∫ 0 ∞ ρ ( r ) 4 π r 2 d r, in the metric. We will see that the mass density ρ ( r ) of black holes is related to a noncommutative parameter or a minimal length.We emphasize that the metric solution (1), as was shown in [33], is associated with the following modified energy-momentum tensor:(3) T μ ν = p ⊥ δ μ ν + p ⊥ + ρ u μ u ν - l μ l ν ,where u μ = g r r δ 0 μ, l μ = ( 1 / g r r ) δ r μ, and p ⊥ = - ρ - ( r / 2 ) ( d ρ / d r ). Note that the appearance of the extra term l μ l ν implies that the modified energy-momentum tensor describes a kind of anisotropic fluid rather than the perfect fluid. As a special case, when the point-like matter is taken, that is, ρ ( r ) = ( M / 2 π r 2 ) δ ( r ), one can retrieve the ordinary Schwarzschild-AdS solution by solving the modified Einstein equations rather than the Einstein equations.


### 2.1. Analogy between the Extreme Black Hole and the Ground State

According to our proposal, we take the probability density of the ground state of a hydrogen atom,| Ψ 100 | 2 = 1 / π a 0 3 exp ⁡ ( - 2 r / a 0 ), where a 0 is the Bohr radius, as the mass density for the extreme black hole(4) ρ 1 r = M 1 π a 3 exp ⁡ - 2 r a ,where M 1 is the total mass of the extreme black hole and a is a parameter that will be seen to be associated with the horizon radius of the extreme black hole, that is, the minimal length in our model. We notice that the specific analogy between | Ψ 100 | 2 and ρ 1 ( r ) is a 0 ~ a.Substituting (4) into (2), we obtain the mass distribution of the extreme black hole(5) M 1 r = M 1 1 - 1 + 2 r a + 2 r 2 a 2 exp ⁡ - 2 r a .One can see from (1) and (5) that the metric singularity at r = 0 has been canceled, which is consistent with the nonlocal gravity [46]. In addition, from g 00 = 0 we deduce the relation between the total mass M 1 and the horizon radius r H as follows:(6) M 1 = r H 2 1 + r H 2 b 2 1 - 1 + 2 r H a + 2 r H 2 a 2 exp ⁡ - 2 r H a - 1 ,which is plotted in Figure 1.Figure 1
The blue curve corresponds to the relation equation (6) that gives the relation between the mass and the horizon of the extreme self-regular Schwarzschild-AdS black hole, and the red curve corresponds to the usual relation associated with the ordinary Schwarzschild-AdS black hole. When the horizon radius grows up, the two curves gradually approach, which means that the effect of noncommutativity mainly exists in the near extremal horizon. Here we set b = 5 a, which satisfies the hoop conjecture; see the analysis under (9) for the details.We can observe in Figure1 that there are two horizon radii in general but, for the extreme case where the mass takes the minimal value M 1 m i n, there is only one horizon radius, the extremal horizon radius r H 1. As r H 1 implies the minimal length, no horizon radius can approach zero. This is the characteristic of the self-regular black hole.By requiring∂ M 1 / ∂ r H = 0, we find that the extremal horizon radius r H 1 that corresponds to M 1 m i n satisfies the following equation:(7) 4 r H 1 5 a 5 + 6 r H 1 4 a 4 + 6 r H 1 3 a 3 + 3 r H 1 2 a 2 1 - exp ⁡ 2 r H 1 a + b 2 a 2 4 r H 1 3 a 3 + 2 r H 1 2 a 2 + 2 r H 1 a + 1 - exp ⁡ r H 1 a = 0 ,where r H 1 can be regarded as the minimal length in our model. As (7) is a transcendental equation, one cannot solve it analytically. Therefore, we make a numerical fitting in terms of the rational fractional function(8) r H 1 a = 1.692 b / a 3 + 2.766 b / a 2 + 20.03 b / a - 7.562 b / a 3 + 1.635 b / a 2 + 15.94 b / a + 3.198 .We plot (7) and its numerical fitting equation (8) for different ratios b / a in Figure 2 from which we can see that the relative error is very small.Figure 2
The numerical points of (7) are plotted in blue color, and the fitting curve of (8) is plotted in red color. The relative error is less than 4 × 1 0 - 5 %.We now analyze theb-parameter dependence of the horizon radius of the extreme black hole.(i)
Ifb ≫ a, which means an asymptotic Minkowski background, we compute from (7) and (6) the extremal horizon radius r H 1 ≈ 1.69182 a and its corresponding minimal mass M 1 m i n ≈ 1.28735 a. (ii)
In order to ensure the formation of a black hole, the hoop conjecture should be considered; that is, the mean radius of a black hole related to some mass distribution should not be larger than the horizon radius of the relevant extreme black hole. The mean radius for the mass density equation (4) reads(9) r - = ∫ 0 ∞ r ρ 1 r 4 π r 2 d r = 3 2 a .Thus, the hoop conjecture requires r H 1 ≥ ( 3 / 2 ) a, whose lower bound gives the corresponding minimal mass M 1 m i n ≈ 1.41728 a. When we consider (7) or (8), the loop conjecture also implies the inequality of the ratio b / a; that is, b / a ≥ 4.99822.As a result, when theb-parameter of the AdS background spacetime meets the hoop conjecture, that is, 4.99822 ≤ b / a < ∞, the horizon radius of the extreme black hole takes the following range:(10) 3 2 ≤ r H 1 a < 1.69182 ,and then the corresponding mass of the extreme black hole is constrained in the range 1.28735 a < M 1 m i n ≤ 1.41728 a. (We notice that for the extreme black hole a small radius corresponds to a large mass, and vice versa. The reason is that a small radius corresponds to a small b-parameter which gives rise to the large pressure P, P ∝ 1 / b 2, and thus an extreme black hole with a small horizon radius has a high mass density and naturally it is heavier than an extreme black hole with a large horizon radius.) This implies that the AdS radius cannot be too small or the curvature of the background spacetime cannot be too large. Moreover, although b has a wide range, r H 1 / a has a narrow one. That is, r H 1 / a correlates weakly with b. As mentioned above, we may take l 0 = ( 3 / 2 ) a as the minimal length which appears naturally from the horizon radius of the extreme black hole.


### 2.2. Analogy between Nonextreme Black Holes and Excited States

In accordance with our proposal mentioned in Section2.1, we take the probability densities of excited states of hydrogen atoms as the mass densities of nonextreme black holes. As our black hole is nonrotational, we choose the probability densities of excited states with no angular momenta | Ψ n 00 | 2 to be the desired mass densities ρ n ( r ) (11) ρ n r = M n π n 5 a 3 ∑ k = 0 n - 1 n ! n - k - 1 ! k + 1 ! k ! - 2 r n a k 2 exp ⁡ - 2 r n a ,where n is a positive integer and M n is the total mass of the nonextreme black hole related to the nth energy level of excited states with no angular momenta. This formula includes the ground state to be the special case of n = 1. Although such a choice of the mass densities for nonextreme black holes will lead to multihorizon solutions, there is no evidence that both the extreme and nonextreme black holes would be monohorizontal, and this choice provides a unified source of black hole mass distributions for both the extreme and the nonextreme cases.Substituting (11) into (2), we compute the mass distributions of nonextreme black holes with n ≥ 2 (12) M 2 r = M 2 1 - 1 + r a + r 2 2 a 2 + r 4 8 a 4 exp ⁡ - r a , M 3 r = M 3 1 - 1 + 2 r 3 a + 2 r 2 9 a 2 + 4 r 4 81 a 4 - 8 r 5 729 a 5 + 8 r 6 6561 a 6 e x p - 2 r 3 a , M 4 r = M 4 1 - 1 + r 2 a + r 2 8 a 2 + 3 r 4 128 a 4 - r 5 128 a 5 + 13 r 6 9216 a 6 - r 7 9216 a 7 + r 8 294912 a 8 e x p - r 2 a , ⋮Setting the largest real root r H n of g 00 = 0 being the horizon radius of the nth nonextreme black hole, we express the total mass M n in terms of the corresponding horizon radius r H n (13) M 2 = r H 2 2 1 + r H 2 2 b 2 1 - 1 + r H 2 a + r H 2 2 2 a 2 + r H 2 4 8 a 4 exp ⁡ - r H 2 a - 1 , M 3 = r H 3 2 1 + r H 3 2 b 2 1 - 1 + 2 r H 3 3 a + 2 r H 3 2 9 a 2 + 4 r H 3 4 81 a 4 - 8 r H 3 5 729 a 5 + 8 r H 3 6 6561 a 6 exp ⁡ - 2 r H 3 3 a - 1 , M 4 = r H 4 2 1 + r H 4 2 b 2 1 - 1 + r H 4 2 a + r H 4 2 8 a 2 + 3 r H 4 4 128 a 4 - r H 4 5 128 a 5 + 13 r H 4 6 9216 a 6 - r H 4 7 9216 a 7 + r H 4 8 294912 a 8 e x p - r H 4 2 a - 1 , ⋮We are now ready to quantize M n by means of quantization of r H n.


## 2.1. Analogy between the Extreme Black Hole and the Ground State

According to our proposal, we take the probability density of the ground state of a hydrogen atom,| Ψ 100 | 2 = 1 / π a 0 3 exp ⁡ ( - 2 r / a 0 ), where a 0 is the Bohr radius, as the mass density for the extreme black hole(4) ρ 1 r = M 1 π a 3 exp ⁡ - 2 r a ,where M 1 is the total mass of the extreme black hole and a is a parameter that will be seen to be associated with the horizon radius of the extreme black hole, that is, the minimal length in our model. We notice that the specific analogy between | Ψ 100 | 2 and ρ 1 ( r ) is a 0 ~ a.Substituting (4) into (2), we obtain the mass distribution of the extreme black hole(5) M 1 r = M 1 1 - 1 + 2 r a + 2 r 2 a 2 exp ⁡ - 2 r a .One can see from (1) and (5) that the metric singularity at r = 0 has been canceled, which is consistent with the nonlocal gravity [46]. In addition, from g 00 = 0 we deduce the relation between the total mass M 1 and the horizon radius r H as follows:(6) M 1 = r H 2 1 + r H 2 b 2 1 - 1 + 2 r H a + 2 r H 2 a 2 exp ⁡ - 2 r H a - 1 ,which is plotted in Figure 1.Figure 1
The blue curve corresponds to the relation equation (6) that gives the relation between the mass and the horizon of the extreme self-regular Schwarzschild-AdS black hole, and the red curve corresponds to the usual relation associated with the ordinary Schwarzschild-AdS black hole. When the horizon radius grows up, the two curves gradually approach, which means that the effect of noncommutativity mainly exists in the near extremal horizon. Here we set b = 5 a, which satisfies the hoop conjecture; see the analysis under (9) for the details.We can observe in Figure1 that there are two horizon radii in general but, for the extreme case where the mass takes the minimal value M 1 m i n, there is only one horizon radius, the extremal horizon radius r H 1. As r H 1 implies the minimal length, no horizon radius can approach zero. This is the characteristic of the self-regular black hole.By requiring∂ M 1 / ∂ r H = 0, we find that the extremal horizon radius r H 1 that corresponds to M 1 m i n satisfies the following equation:(7) 4 r H 1 5 a 5 + 6 r H 1 4 a 4 + 6 r H 1 3 a 3 + 3 r H 1 2 a 2 1 - exp ⁡ 2 r H 1 a + b 2 a 2 4 r H 1 3 a 3 + 2 r H 1 2 a 2 + 2 r H 1 a + 1 - exp ⁡ r H 1 a = 0 ,where r H 1 can be regarded as the minimal length in our model. As (7) is a transcendental equation, one cannot solve it analytically. Therefore, we make a numerical fitting in terms of the rational fractional function(8) r H 1 a = 1.692 b / a 3 + 2.766 b / a 2 + 20.03 b / a - 7.562 b / a 3 + 1.635 b / a 2 + 15.94 b / a + 3.198 .We plot (7) and its numerical fitting equation (8) for different ratios b / a in Figure 2 from which we can see that the relative error is very small.Figure 2
The numerical points of (7) are plotted in blue color, and the fitting curve of (8) is plotted in red color. The relative error is less than 4 × 1 0 - 5 %.We now analyze theb-parameter dependence of the horizon radius of the extreme black hole.(i)
Ifb ≫ a, which means an asymptotic Minkowski background, we compute from (7) and (6) the extremal horizon radius r H 1 ≈ 1.69182 a and its corresponding minimal mass M 1 m i n ≈ 1.28735 a. (ii)
In order to ensure the formation of a black hole, the hoop conjecture should be considered; that is, the mean radius of a black hole related to some mass distribution should not be larger than the horizon radius of the relevant extreme black hole. The mean radius for the mass density equation (4) reads(9) r - = ∫ 0 ∞ r ρ 1 r 4 π r 2 d r = 3 2 a .Thus, the hoop conjecture requires r H 1 ≥ ( 3 / 2 ) a, whose lower bound gives the corresponding minimal mass M 1 m i n ≈ 1.41728 a. When we consider (7) or (8), the loop conjecture also implies the inequality of the ratio b / a; that is, b / a ≥ 4.99822.As a result, when theb-parameter of the AdS background spacetime meets the hoop conjecture, that is, 4.99822 ≤ b / a < ∞, the horizon radius of the extreme black hole takes the following range:(10) 3 2 ≤ r H 1 a < 1.69182 ,and then the corresponding mass of the extreme black hole is constrained in the range 1.28735 a < M 1 m i n ≤ 1.41728 a. (We notice that for the extreme black hole a small radius corresponds to a large mass, and vice versa. The reason is that a small radius corresponds to a small b-parameter which gives rise to the large pressure P, P ∝ 1 / b 2, and thus an extreme black hole with a small horizon radius has a high mass density and naturally it is heavier than an extreme black hole with a large horizon radius.) This implies that the AdS radius cannot be too small or the curvature of the background spacetime cannot be too large. Moreover, although b has a wide range, r H 1 / a has a narrow one. That is, r H 1 / a correlates weakly with b. As mentioned above, we may take l 0 = ( 3 / 2 ) a as the minimal length which appears naturally from the horizon radius of the extreme black hole.


## 2.2. Analogy between Nonextreme Black Holes and Excited States

In accordance with our proposal mentioned in Section2.1, we take the probability densities of excited states of hydrogen atoms as the mass densities of nonextreme black holes. As our black hole is nonrotational, we choose the probability densities of excited states with no angular momenta | Ψ n 00 | 2 to be the desired mass densities ρ n ( r ) (11) ρ n r = M n π n 5 a 3 ∑ k = 0 n - 1 n ! n - k - 1 ! k + 1 ! k ! - 2 r n a k 2 exp ⁡ - 2 r n a ,where n is a positive integer and M n is the total mass of the nonextreme black hole related to the nth energy level of excited states with no angular momenta. This formula includes the ground state to be the special case of n = 1. Although such a choice of the mass densities for nonextreme black holes will lead to multihorizon solutions, there is no evidence that both the extreme and nonextreme black holes would be monohorizontal, and this choice provides a unified source of black hole mass distributions for both the extreme and the nonextreme cases.Substituting (11) into (2), we compute the mass distributions of nonextreme black holes with n ≥ 2 (12) M 2 r = M 2 1 - 1 + r a + r 2 2 a 2 + r 4 8 a 4 exp ⁡ - r a , M 3 r = M 3 1 - 1 + 2 r 3 a + 2 r 2 9 a 2 + 4 r 4 81 a 4 - 8 r 5 729 a 5 + 8 r 6 6561 a 6 e x p - 2 r 3 a , M 4 r = M 4 1 - 1 + r 2 a + r 2 8 a 2 + 3 r 4 128 a 4 - r 5 128 a 5 + 13 r 6 9216 a 6 - r 7 9216 a 7 + r 8 294912 a 8 e x p - r 2 a , ⋮Setting the largest real root r H n of g 00 = 0 being the horizon radius of the nth nonextreme black hole, we express the total mass M n in terms of the corresponding horizon radius r H n (13) M 2 = r H 2 2 1 + r H 2 2 b 2 1 - 1 + r H 2 a + r H 2 2 2 a 2 + r H 2 4 8 a 4 exp ⁡ - r H 2 a - 1 , M 3 = r H 3 2 1 + r H 3 2 b 2 1 - 1 + 2 r H 3 3 a + 2 r H 3 2 9 a 2 + 4 r H 3 4 81 a 4 - 8 r H 3 5 729 a 5 + 8 r H 3 6 6561 a 6 exp ⁡ - 2 r H 3 3 a - 1 , M 4 = r H 4 2 1 + r H 4 2 b 2 1 - 1 + r H 4 2 a + r H 4 2 8 a 2 + 3 r H 4 4 128 a 4 - r H 4 5 128 a 5 + 13 r H 4 6 9216 a 6 - r H 4 7 9216 a 7 + r H 4 8 294912 a 8 e x p - r H 4 2 a - 1 , ⋮We are now ready to quantize M n by means of quantization of r H n.


## 3. Quantization of Extreme and Nonextreme Black Holes

In [40] the mass of black holes is quantized directly because the self-regular Schwarzschild black hole is regarded as the quantum harmonic oscillator. Here the situation is different. Our proposal, based on the works by Corda [41–44] and Bekenstein [45], is the analogue of the self-regular Schwarzschild-AdS black hole and the hydrogen atom with no angular momenta. Thus, we are inclined to adopt quantization of horizons. Specifically, for the hydrogen atom with no angular momenta, its quantum mean radius reads 〈 r 〉 = ( 3 a 0 / 2 ) n 2 ∝ n 2. Because the mean radius of hydrogen atoms corresponds to the horizon radius of black holes, the quantum horizon radius of the self-regular Schwarzschild-AdS black hole is naturally assumed to be(14) r H n = n 2 r H 1 ,where r H 1 is, like a 0 in hydrogen atoms, the horizon radius of the extreme black hole. Substituting (14) into (6) and (13), we obtain the quantized masses of the extreme and nonextreme black holes that are expressed in terms of the extremal horizon radius or the minimal length r H 1 (15) M 1 m i n = r H 1 2 1 + r H 1 2 b 2 1 - 1 + 2 r H 1 a + 2 r H 1 2 a 2 exp ⁡ - 2 r H 1 a - 1 , M 2 quan = 2 r H 1 1 + 16 r H 1 2 b 2 1 - 1 + 4 r H 1 a + 8 r H 1 2 a 2 + 32 r H 1 4 a 4 exp ⁡ - 4 r H 1 a - 1 , M 3 q u a n = 9 r H 1 2 1 + 81 r H 1 2 b 2 1 - 1 + 6 r H 1 a + 18 r H 1 2 2 a 2 + 324 r H 1 4 a 4 - 648 r H 1 5 a 5 + 648 r H 1 6 a 6 exp ⁡ - 6 r H 1 a - 1 , M 4 q u a n = 8 r H 1 1 + 256 r H 1 2 b 2 1 - 1 + 8 r H 1 a + 32 r H 1 2 a 2 + 1536 r H 1 4 a 4 - 8192 r H 1 5 a 5 + 212992 r H 1 6 9 a 6 - 262144 r H 1 7 9 a 7 + 131072 r H 1 8 9 a 8 exp ⁡ - 8 r H 1 a - 1 , ⋮We plot (6) and (13) in Figure 3, where the four black round points denote the quantized masses of the extreme black hole (M 1 m i n) and the nonextreme black holes (M n q u a n,  n = 2,3 , 4), respectively.Figure 3
Plots of the relations between black hole masses and their horizon radii. The blue, red, orange, and green curves correspond to the cases ofn = 1,2 , 3,4, respectively, where we set b / a = 5 which has been verified to satisfy the hoop conjecture; see (9).Now we turn to the discussion of the quantum hoop conjecture which has the following form [40]:(16) n r n ≤ n r H n n .Considering (11) and (14), we calculate (17) n r n = ∫ 0 ∞ r ρ n r M n 4 π r 2 d r = 3 2 a n 2 , n r H n n = ∫ 0 ∞ r H n ρ n r M n 4 π r 2 d r = n 4 r H 1 .As a result, the quantum hoop conjecture in our proposal reads (18) 3 2 a ≤ n 2 r H 1 .For the extreme black hole, that is, the case n = 1, the quantum hoop conjecture is satisfied because it reduces to (10). For the nonextreme black holes, that is, the case n ≥ 2, the quantum hoop conjecture is obviously satisfied. This means that our assumption of quantization, see (14), coincides with the quantum hoop conjecture. That is to say, the black holes can be formed at the quantum level in our proposal.As to the Correspondence Principle, it usually indicates a transition from quantum theory to classical theory. In quantum mechanics, there are two alternatives to realize such a transition. One is the limit of a large quantum number, and the other is the limit ofħ → 0. The latter alternative corresponds to the limit of a → 0 in our proposal, which implies the fact that the minimal length (l 0 = ( 3 / 2 ) a) can be neglected for a black hole with a large scale. We can check that when a → 0, the mass densities (11) turn back to the δ ( r )-function density that describes, from the point of view of the modified Einstein equations, the ordinary Schwarzschild-AdS black hole without the effect of the minimal length. Consequently, the Correspondence Principle is satisfied in our proposal of black hole quantization.


## 4. Summary

Based on the recent works by Corda [41–44] and Bekenstein [45], the analogue of a self-regular Schwarzschild-AdS black hole and a hydrogen atom is assumed. Correspondingly, the quantization of horizons is utilized. In this way, the total mass of a self-regular Schwarzschild-AdS black hole is quantized. Moreover, the quantum hoop conjecture and the Correspondence Principle are verified in our proposal.



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