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ORIGINAL RESEARCH article

Front. Astron. Space Sci., 11 June 2021 | https://doi.org/10.3389/fspas.2021.647241

Loop Quantum Black Hole Extensions Within the Improved Dynamics

  • 1Department of Physics, University of the Republic, Montevideo, Uruguay
  • 2Departamento de Física Teórica y Del Cosmos, Universidad de Granada, Granada, Spain
  • 3Department of Physics and Astronomy, Louisiana State University, Baton Rouge, LA, United States

We continue our investigation of an improved quantization scheme for spherically symmetric loop quantum gravity. We find that in the region where the black hole singularity appears in the classical theory, the quantum theory contains semi-classical states that approximate general relativity coupled to an effective anisotropic fluid. The singularity is eliminated and the space-time can be continued into a white hole space-time. This is similar to previously considered scenarios based on a loop quantum gravity quantization.

1 Introduction

In a previous paper (Gambini et al., 2020a) we studied an improved quantization for spherically symmetric loop quantum gravity. Earlier work (Gambini and Pullin, 2013; Gambini et al., 2014; Gambini et al., 2020b) had considered a constant polymerization parameter, similarly to the “μ0” quantization scheme in loop quantum cosmology, whereas the improved quantization is similar to the “μ¯” quantization scheme (Ashtekar and Singh, 2011). Other approaches involving improved quantizations have also been explored in (Han and Liu, 2020). We observed that the singularity was removed, but we did not analyze in detail what happened to the space-time beyond the region where the singularity used to be. Here we complete that study. We find that in that region there exist semi-classical quantum states for which the theory behaves like a quantum version of general relativity coupled to an effective anisotropic fluid (Cho and Kim, 2019) that violates the dominant energy condition. In the highest curvature region there is a space-like transition surface, something that was unnoticed in (Gambini et al., 2020a). The space-time continues into a white hole geometry, like in Ref. (Ashtekar et al., 2018). However, in this work we consider a different regularization for the parametrized observable associated to the shift function. Its very definition requires the choice of a slicing and the new regularization avoids an undesirable dependence on it in the semiclassical limit.

The organization of this paper is as follows. In section 2 we discuss the physical sector of the quantum theory, focusing on semiclassical sectors. In section 3 we introduce a horizon penetrating slicing based on Painlevé–Gullstrand coordinates and show how it can be used to connect to a white hole space-time. We end with a discussion.

2 Physical Sector of the Quantum Theory

The physical sector of the theory is obtained after combining Loop Quantum Gravity quantization techniques and the Dirac quantization program for constrained theories. In summary, we start with a kinematical Hilbert space in the loop representation adapted to spherically symmetric spacetimes for the geometrical sector [(Kφ,Eφ),(Kx,Ex)] together with a standard representation for the spacetime mass and its conjugate momentum (M,PM). A suitable basis of kinematical states is the one provided by spherical symmetric spin networks tensor product with the standard states for the matter sector in the mass representation. Then, we represent the scalar constraint as a well-defined operator in the kinemtical Hilbert space (for the diffeomorphism constraint we rather work with the related finite group of transformations mimicking the full theory).

Following the construction of Ref. (Gambini et al., 2020a), the physical sector of the theory is encoded in physical states (solutions to the scalar constraint) endowed with a suitable inner product and a set of physical observables. This is achieved, for instance, by applying group averaging techniques for both the quantum scalar constraint and the group of finite spatial diffeomorphisms (see also Refs (Gambini and Pullin, 2013; de Blas et al., 2017)). We focus our study to some of the simplest semi-classical states. Quantum states consist of spatial spin networks labeled by the ADM mass M (a Dirac observable) and integer numbers that characterize the radii of spheres of symmetry associated with each vertex of the network ki. The semi-classical states we are going to consider here are given by superpositions in the mass centered at M0 and of width δM0 and are therefore associated with a fixed discrete structure in space (see (Gambini et al., 2020a) for more details). They provide excellent approximations to the classical geometry in regions of small curvature compared to Planck scale. Concretely, we consider the semi-classical states

|ψ=1δM0dMeiMP0/cos[π(MM0)2δM0]Θ(MM0+δM0)Θ(M0+δM0M)×|M,kS,,k0,,kS(2.1)

with k0<kj for all j0, namely, j=S,S+1,,1,1,,S, where

k0=Int[(2GM0Δ4πPl3)2/3],(2.2)

times the Planck length squared determines the smallest area of the 2-spheres in the theory. This corresponds to the improved quantization, where Δ is the area gap. Besides, we choose M0mPl and

δM032(4πPl32GΔ)2/3M01/3.(2.3)

The states in Eq. 2.1 belong to a family of sharply peaked semiclassical states in the mass and with support on a concrete spin network (states with higher dispersion in the mass will require superpositions of different spin networks). This choice considerably simplifies the analysis of the effective geometries. As we discussed in our previous papers, the quantum theory has additional observables to the ones encountered in classical treatments (Kastrup and Thiemann, 1994; Kuchar, 1994) which are the ADM mass and the time at infinity. These emerge from the discrete nature of the spin network treatment and are associated with the ki’s, which in turn are associated with the value of the areas of the spheres of symmetry connected with each vertex of the spin network. One can also consider states that are a superposition of M’s. The analysis will remain the same as long as the states are peaked around a value of M.

In addition to physical states, the physical observables representing space-time metric components will be defined through suitable parametrized observables. They act as local operators on each vertex of the spin network. Furthermore, they involve point holonomies that are chosen to be compatible with the superselection sectors of the physical Hilbert space (see Ref (Gambini et al., 2020a). for more details). Some of the basic parametrized observables are

E^x(xj)|M,k=O^(z(xj))|M,k=Pl2kj(xj)|M,k,(2.4)
M^|M,k=M|M,k,(2.5)

where z(x) is a suitable gauge function that codifies the freedom in the choice of radial reparametrizations.

For the components of the space-time metric on stationary slicings we have, for instance, the lapse and shift,1

N^2(xj):=14([E^x(xj)])2(E^φ(xj))2,[N^x(xj)]2=E^x(xj)(E^φ(xj))2sin2(ρ¯jKφ(xj))ρ¯j2^,(2.6)

where

(E^φ(xj))2=[(E^x(xj))]2/41+sin2(ρ¯jKφ(xj))ρ¯j22GM^|E^x(xj)|,(2.7)

where we polymerized Kφ with ρ¯ the polymerization parameter of the improved quantization,

ρ¯=Δ4πE^x.(2.8)

We choose the k’s in the one-dimensional spin network in our physical state and the gauge function z(x) such that

E^x(xj)=Pl2Int[xj2Pl2],(2.9)
[E^x(xj)]|M,k=Pl2δxInt[(xj+δx)2xj2Pl2]|M,k,(2.10)

and with xj=δx|j|+x0 and with j, where

x0=Int[(2GMΔ4π)2/3].(2.11)

Besides, we will choose δx=Pl as in the first paper (Gambini et al., 2020a), although we will discuss the consequences of the limiting choices (for a uniform lattice) δx=Pl22x0 and δx=x0. The different spacings δx just mentioned here correspond to different choices of states in the physical space, all of them lead to the same semiclassical behavior but differ in the deep quantum regime close to the singularity, as one would expect. The quantum regime is for the small values of ki, where if one were to consider a superposition of states, small changes in ki’s would lead to great fluctuations in the properties of the states.

Then, the metric components take the following form in terms of the previous operators

g^tt(xj)=(N^2g^xx[N^x]2),g^tx(xj)=g^xx[N^x]2,
g^xx(xj)=(E^φ)2E^x,gθθ(xj)=E^x,gϕϕ(xj)=E^xsin2θ.

Let us restrict the study to the family of stationary slicings determined by the condition

sin2(ρ¯jKφ(xj))^=[F^(xj)]2(2.12)

where some specific choices of F(xj) will be studied below. However, any viable choice must be such that F(x) is real and F(x)[1,1]. Now, one can easily construct the operators corresponding to the components of the spacetime metric. They are given by

g^tt(xj)=(1r^SE^x),g^tx(xj)=πΔ{[Ex]^}F^21r^SE^x+4πE^xF^2Δ,g^xx(xj)={[Ex]^}24E^x(1r^SE^x+4πE^xF^2Δ),g^θθ(xj)=E^x,g^ϕϕ(xj)=E^xsin2θ,

with r^S=2GM^. The effective metric is defined as gμν=g^μν, where the expectation value is computed on the extended physical state |ψ we presented above. We will focus on the leading order corrections when the dispersion in the mass can be neglected. In this case, we can just remove the hats in the previous expression and denote this contribution by g(0)uv(xj). In addition, we will take a continuum limit that was discussed in our first paper. Namely, xj=δx|j|+x0 is replaced by (|x|+x0), with x and the integer part function Int[] will be dropped from all expressions. This continuum limit means that the effective geometries bounce when they reach x=0.

3 Painlevé-Gullstrand Coordinates: Black Hole to White Hole Transition

We are interested in spatial slicings that are horizon penetrating and asymptotically flat. For instance, ingoing Painlevé-Gullstrand coordinates is one of the well-known choices that meet these requirements. Besides, the time coordinate follows the proper time of a free-falling observer. The slicing is defined by the condition F^(xj)=F^1(xj) where

F^1(xj)=ρ¯r^SE^x.(3.1)

This choice is equivalent to a lapse operator N^(xj)=I^. Besides, one can easily see that in the semiclassical limit xjx+x0 we have the function F1(x)<1 for all x0, while F1(x=0)=1. This is important since this choice will allow us to completely probe the high curvature region of the effective geometries.

They can be obtained as in (Gambini et al., 2020a). One gets

g(0)tt(x)=(1rS|x|+x0),g(0)tx(x)=sign(x)rS|x|+x0(1+δx2(|x|+x0)),g(0)xx(x)=(1+δx2(|x|+x0))2,g(0)θθ(x)=(|x|+x0)2,g(0)ϕϕ(x)=(|x|+x0)2sin2θ.(3.2)

For this slicing, the low curvature regions occur when F(x)0 or equivalently at x±. Concretely, at x+ the effective metric approaches sufficiently fast a classical black hole metric in ingoing Painlevé-Gullstrand coordinates, while for x the effective metric approaches sufficiently fast a classical white hole metric in outgoing Painlevé-Gullstrand coordinates. On the other hand, as we will see below, the curvature reaches its maximum when F(x)=1, namely, at x=0.

In what follows, we refer to Figure 1 (see the similarities with the Penrose diagram of Ref (Ashtekar et al., 2018)). One can see that the condition g(0)tt(x)=0 has two real solutions in x, corresponding to two classical black or white hole horizons, at xBH>0 and xWH<0. In the spacetime regions with x>xBH or x<xWH, the surfaces x=const are time-like, and correspond to untrapped regions. In the region right behind the black hole horizon, x<xBH, x=const hypersurfaces are space-like. This region is a trapped black hole interior. As we move toward the high curvature region, curvature is maximum at x=0. This space-like hypersurface connects the trapped black hole region with an anti-trapped white hole region. This is the so-called transition surface (Ashtekar et al., 2018). The anti-trapped white hole region extends all the way from x=0 to the white hole horizon x=xWH. In all this region, x=const hypersurfaces are still space-like. Once the white hole horizon x=xWH is crossed to the outside region, spacetime is untrapped again and x=const hypersurfaces are again time-like.

FIGURE 1
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FIGURE 1. Penrose diagram of the effective geometry determined by the slicing in Eq. 3.1. Black and green lines indicate low and high curvature regions, respectively. Continuous lines represent smooth regions while dotted lines are associated to a discrete geometry. Dashed lines indicate that the spacetime diagram continues up and down.

In order to illustrate all these properties, it is convenient to first write the effective metric in its diagonal form (It should be noted that although the theory does not recover the full diffeomorphism invariance of the classical theory in the quantum regions, it is a valid mathematical tool to diagonalize a metric nevertheless.) It can be easily obtained by introducing the change of coordinates

dtdt+g(0)tx(x)g(0)tt(x)dx(3.3)

This transformation amounts to the change

g(0)xx(x)g˜(0)xx(x)=(1+δx2(|x|+x0))2(1rS|x|+x0),g(0)tx(x)g˜(0)tx(x)=0,(3.4)

while all other components remain as

g(0)tt(x)g˜(0)tt(x)=(1rS|x|+x0),(3.5)
g(00)θθ(x)g˜(00)θθ(x)=(|x|+x0)2,g˜(00)φφ(x)g˜(00)φφ(x)=(|x|+x0)2sinθ.(3.6)

In Figure 2 we show two components of the effective metric in its diagonal form. There where they vanish, a horizon forms and the coordinate system becomes singular. However, we should remember that around xx0 spacetime is discrete and the continuous line is just an interpolation. Therefore, the metric will be well defined provided the horizons are not located on a vertex of the lattice.

FIGURE 2
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FIGURE 2. The values of the tt component of the metric and the inverse of xx for the metric in diagonal form. When the first vanishes, horizons arise. Notice that in the region between the two horizons the discreteness is significant as represented in the separation of the dots (although in the plot we do not show all the points in the lattice but only one out of fifty).

We have also studied the effective stress-energy tensor that encodes the main deviations from the classical theory. It is defined as

Tμν:=18πGGμν,(3.7)

where Gμν is the Einstein tensor. Tμν is characterized by the effective energy density ρ and radial and tangential pressures densities, px and p||, respectively. They are defined by means of

ρext:=TμνXμXνXρXρ,(3.8)
pxext:=Tμνrμrνrρrρ,(3.9)

and

p||ext:=Tμνθμθνθρθρ,(3.10)

where Xμ is the Killing vector field that is time-like in the regions in which x=const hypersurfaces are time-like. rμ and θμ are the vector fields pointing in the radial and θ-angular directions, respectively. When the Killing vector field Xμ is space-like, namely, in the regions in which x=const hypersurfaces are space-like, rμ becomes time-like. Therefore,

ρint:=Tμνrμrνrρrρ,(3.11)
pxint:=TμνXμXνXρXρ,(3.12)

while p||int=p||ext since θμ remains space-like. We will assume that these effective space-times can be approximated by a smooth and continuous geometry everywhere, even at the transition surface. This assumption, as we mentioned, fails in the most quantum region. However, we expect that Tμν (a quantity only valid when geometry is smooth) will still give us qualitative hints about quantum geometry corrections there.

In Figure 3 we show the components of the stress-energy tensor Tμν, or equivalently, the components of the Einstein tensor (up to a factor (8πG)) for the choice δx=Pl. From them it is easy to extract the energy densities and pressures in each region of these effective space-times.

FIGURE 3
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FIGURE 3. The stress energy tensor of the effective metric g˜(0)μv(x). This plot corresponds to δx=Pl, namely, s=1.

It is straightforward to compute the value of the energy density and pressures of the stress-energy tensor at the transition surface and in the limit of large mass rSPl. Actually, their value depend on the choice of spacing δx of the uniform lattice in the radial direction. For instance, for δx=x0(Plx0)s with s=0,1,2, one can see that2

ρint(x=0)=2πΔ×O([Δ2πrS]s/3+2/3),pxint(x=0)=2πΔ×O([Δ2πrS]s/3),p||int(x=0)=2πΔ×O([Δ2πrS]s/3)(3.13)

Let us note that in the most quantum region,

ωx(x=0)=pxint(x=0)ρint(x=0)=O([2πrSΔ]2/3),ω||(x=0)=p||int(x=0)ρint(x=0)=O([2πrSΔ]2/3).(3.14)

As we see, at the transition surface, the effective stress-energy tensor does not violate the strong energy condition since ρint(x=0)0. However, it does actually violate the dominant energy condition. Since the dominant energy condition implies that |ωx|1 and |ω|||1, we conclude that this condition is violated since both |ωx(x=0)| and |ω||(x=0)| at the transition quantum spacetime blow up in the limit rSPl.

One can construct the Penrose diagram of this geometry, together with a possible extension to regions not covered by our slicing.

4 Discussion

There are several comments about the scenario studied in this manuscript. On the one hand, the effective geometries that one can derive in this theory are uniquely determined by the semiclassical physical state and the (parameterized) observables that represent the components of the metric. The quantum corrections on these geometries likewise depend on the minimal area gap Δ and the size of the discretization of the physical states we are considering. Polymer corrections due to the choice of foliation will also contribute if fluctuations of the mass are considered. We are taking for simplicity an element (spin network) of the basis in the physical space of states and ignoring superpositions in different discretizations and masses. Quantum corrections break the covariance, in particular because their dependence on the discretization of the chosen quantum states, but also due to foliation dependent terms. The latter produce O(ΔrS2/x2) quantum corrections in the (asymptotically flat) external region of the black hole and therefore they are completely unobservable for macroscopic black holes, allowing to recover diffeomorphism invariance. Since different foliations are identified with (observer’s) frames of reference, this is equivalent to say that, for physically implementable frames of reference (i.e. physically realizable observers) in the exterior region, quantum corrections will be negligible. Nevertheless, these quantum corrections increase when approaching the high curvature region, reaching maximum values of order O(ΔrS2/x02). For instance, a free-falling observer (as it is the case under consideration in this manuscript) and an accelerated observer will observe there only slightly different corrections, even if its foliation involves accelerations that are Planck order.

Regarding the original choice of shift as parametrized observable adopted in Ref. (Gambini et al., 2020a), we noticed that, as mentioned in (Kelly et al., 2020), the most quantum region showed an inner Cauchy horizon connecting the trapped black hole region with a Planckian size transition space-time where x=const hypersurfaces are time-like. However, strictly speaking, due to this Cauchy horizon, the extension beyond this region is not unique. After the bounce a Cauchy Horizon is traversed and therefore the initial conditions at that end up producing a black hole are not enough for the determination of the possible extensions beyond the Cauchy horizon. Notice that the Cauchy horizon occurs in a deep quantum region that is in the past of the extension; further non-uniqueness would occur when quantum superpositions are considered. Besides, different foliations capture different extensions. We saw that a choice of foliation (corresponding to an accelerated observer with a Planck order acceleration) leads to an anti de Sitter universe beyond the Cauchy horizon. Similar ambiguities have been noted in classical general relativity (Dafermos and Luk, 2017). One must keep in mind that these ambiguities can be alleviated by considering parametrized observables that correspond to physically implementable frames of reference (i.e. physically realizable observers). We are considering here extrinsic framings corresponding to a choice of polimerization for the functional parameter Kφ(xj). Even though the theory is covariant in the sense that the classical observables become quantum observables in the quantization process, each polimerization corresponds to a different choice of framing. In reference (Gambini and Pullin, 2009) we proved that diffeomorphism invariance of the parametrized observables corresponding to the metric is only preserved for diffeomorphism that do not amplify Planck scale separation to macroscopic scale. The introduction of more realistic intrinsic framings resulting from the inclusion of matter would provide a natural choice of slicing allowing to solve this limitation. For instance, the case of Painlevé-Gullstrand coordinates, that amount to a unit parametrized observable related to the lapse function. The kind of midisuperspace model here considered allows to analyze this issues while most of the minisuperspace scenarios proposed in the literature (see (Bodendorfer et al., 1912; Sartini and Geiller, 2021; Boehmer and Vandersloot, 2007; Campiglia et al., 2008; Ashtekar and Singh, 2011; Cortez et al., 2017; Olmedo et al., 2017; Alesci et al., 2018; Alesci et al., 2019; Assanioussi et al., 2020) for references on hypersurface orthogonal slicings) adopted a particular family of space-time foliations where this issue of slicing dependence did not arise. Other authors have taken the issue of non-covariance to imply that modifications of the constraint algebra are in order, leading to the deformed hypersurface deformation algebra approach (Tibrewala, 2012; Bojowald et al., 2015; Ben Achour et al., 2018).

Summarizing, we have applied an improved quantization scheme for loop quantum gravity in spherical symmetry. The singularity that appears in classical general relativity is eliminated and space-time is continued to a white hole space-time geometry through a transition surface where curvature reaches its maximum value. This is qualitatively similar to scenarios that have been recently proposed (Ashtekar et al., 2018). Our proposal yields effective geometries that are free of undesirable slicing dependencies in the semiclassical limit. Actually, the slicing independence in a precise semiclassical limit of small mass fluctuations can be invoked to restrict polymer modifications of the scalar constraint and the parametrized observables describing the quantum geometry. Finally, it is interesting to note that most of the ideas presented here and in Ref (Gambini et al., 2020a). can be very useful in other situations, like in the vacuum polarized T3 Gowdy cosmologies with local rotational symmetry (de Blas et al., 2017).

Data Availability Statement

The original contributions presented in the study are included in the article/Supplementary Material, further inquiries can be directed to the corresponding author.

Author Contributions

All authors collaborated equally in the research and elaboration of the manuscript.

Conflict of Interest

The authors declare that the research was conducted in the absence of any commercial or financial relationships that could be construed as a potential conflict of interest.

Acknowledgments

This work was supported in part by Grant NSF-PHY-1903799, funds of the Hearne Institute for Theoretical Physics, CCT-LSU, Pedeciba, Fondo Clemente Estable FCE_1_2019_1_155865 and Project. No. FIS 2017–86497-C2-2-P of MICINN from Spain. J.O. acknowledges the Operative Program FEDER2014–2020 and the Consejería de Economía y Conocimiento de la Junta de Andalucía.

Footnotes

1In Ref (Gambini et al., 2020a). for the shift we adopted the regularization Kφ(xj)sin(2ρ¯jKφ(xj))/2ρ¯j, but it introduces an undesirable slicing dependence that is avoided with the present regularization. Besides, the representation that we adopt here for the square of the shift function as a parametrized observable is compatible with the superselection rules of the quantum numbers νj of the kinematical spin networks as it was discussed in Ref. (Gambini et al., 2020a).

2The choices of δx shown here correspond to the maximum allowed uniform discretization if s=0, while s=2 gives the finest uniform refinement. s=1 is an intermediate choice.

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Keywords: loop quantum gravity, black holes, quantum field theory, spin networks, general relativity

Citation: Gambini R, Olmedo J and Pullin J (2021) Loop Quantum Black Hole Extensions Within the Improved Dynamics. Front. Astron. Space Sci. 8:647241. doi: 10.3389/fspas.2021.647241

Received: 29 December 2020; Accepted: 26 April 2021;
Published: 11 June 2021.

Edited by:

Francesca Vidotto, Western University, Canada

Reviewed by:

Jibril Ben Achour, Ludwig-Maximilians-University Munich, Germany
Kristina Giesel, University of Erlangen Nuremberg, Germany
Ana Alonso Serrano, Max Planck Institute for Gravitational Physics (AEI), Germany

Copyright © 2021 Gambini, Olmedo and Pullin. This is an open-access article distributed under the terms of the Creative Commons Attribution License (CC BY). The use, distribution or reproduction in other forums is permitted, provided the original author(s) and the copyright owner(s) are credited and that the original publication in this journal is cited, in accordance with accepted academic practice. No use, distribution or reproduction is permitted which does not comply with these terms.

*Correspondence: Javier Olmedo, javolmedo@ugr.es