Quantum Black Holes and (Re)Solution of the Singularity

Abstract

Classical general relativity predicts the occurrence of spacetime singularities under very general conditions. Starting from the idea that the spacetime geometry must be described by suitable states in the complete quantum theory of matter and gravity, we shall argue that this scenario cannot be realised physically since no proper quantum state may contain the infinite momentum modes required to resolve the singularity.

1. Introduction

Exact solutions to the Einstein field equations containing spacetime singularities have been known since the early days of general relativity. Moreover, the Penrose theorem ensures that the gravitational collapse of compact objects will generate geodesically incomplete spacetimes if a trapping surface occurs [1] (albeit eternal point-like sources were shown to be mathematically incompatible with the Einstein equations [2]).

It is generically expected that the quantum theory of gravity will fix this incomplete classical picture, although no general consensus has yet been reached as to how this happens and on what observable effects that could imply. One of the main difficulties in quantising the gravitational interaction is given by its non-linear nature already at the classical level. Building quantum states corresponding to the real objects that we see in the universe is, therefore, a strongly non-perturbative endeavour.

We will report here on the consequences stemming from the assumptions that (a) the expectation value of quantum gravity observables on states that are relevant for the description of reality must be very close to the classical solutions of the Einstein Equations, where experimental data support general relativity, and (b) those quantum states must be mathematically well-defined. The second assumption implies that not all classical solutions may be realised. A well-known example is the hydrogen atom, which should be unstable according to classical electrodynamics. Instead, quantum mechanics predicts discrete energy states for the electron, with the ground state spreading several orders of magnitude around the size of the nucleus.

The above point of view was taken in Ref. [3] for studying the collapse of a ball of dust of mass M, whose classical radius $R\to 0$ in a finite amount of proper time [4]. The main result that followed was that the ground state is much wider than the Planck length, and indeed of the order of the gravitational radius $R_{\mathrm{H}}=2G_{\mathrm{N}}M$, which appears as a concrete example of classicalisation [5,6]. Moreover, the principal quantum number of the ground state is proportional to $M^2/m_{\mathrm{p}}^2$ (we use units with $c=1$, $G_{\mathrm{N}}={\ell }_{\mathrm{p}}/m_{\mathrm{p}}$ and $\hslash ={\ell }_{\mathrm{p}}{m}_{\mathrm{p}}$, where ${\ell }_{\mathrm{p}}$ is the Planck length and $m_{\mathrm{p}}$ is the Planck mass). This property was also recovered in Ref. [7], in which the existence of a proper quantum state reproducing the outer Schwarzschild geometry was considered to show that no central singularity could be possibly realised. In that context, the scaling of $M^2/m_{\mathrm{p}}^2$ with an integer number can then be interpreted as the quantisation of the horizon area [8].

2. Quantum Dust Ball

The classical Oppenheimer–Snyder model [4] describes the collapse of a ball of dust in general relativity. The trajectory of the areal radius R of the ball is a geodesic in the Schwarzschild spacetime generated by the mass M of the ball itself

$$\begin{array}{c}\hfill \mathrm{d}{s}^2=-\left(1-\frac{R_{\mathrm{H}}}{r}\right)\mathrm{d}{t}^2+{\left(1-\frac{R_{\mathrm{H}}}{r}\right)}^{-1}\mathrm{d}{r}^2+r^2\mathrm{d}{\Omega }^2.\end{array}$$

(1)

Consequently, one obtains the conservation of the effective Hamiltonian [3] (Numerical coefficients of order one are often omitted for the sake of clarity).

$$\begin{array}{c}\hfill H\equiv \frac{P^2}{2M}-\frac{G_{\mathrm{N}}{M}^2}{R}=\frac{M}{2}\left(\frac{E^2}{M^2}-1\right)\equiv \mathcal{E},\end{array}$$

(2)

where P is the momentum conjugated to R and E represents the conserved energy conjugated to the coordinate time t. It is important to remark that Equation (2) formally equals the Newtonian conservation law for the energy $\mathcal{E}$, but the general relativistic equation differs because of the non-linear relation between $\mathcal{E}$ and the energy E.

We next quantise the system by assuming the usual canonical commutator

$$\begin{array}{c}\hfill \left[\widehat{R},\widehat{P}\right]=i\hslash ,\end{array}$$

(3)

and the operators $\widehat{R}$ and $\widehat{P}$ act on wavefunctions $\Psi =\Psi \left(R\right)$ satisfying the Schrödinger equation for a gravitational atom

$$\begin{array}{c}\hfill \widehat{H}\Psi =\mathcal{E}\Psi .\end{array}$$

(4)

The eigenstates of the above equation are given by

$$\begin{array}{c}\hfill {\Psi }_n\simeq e^{-\frac{x}{n}}{L}_{n-1}^1\left(\frac{2x}{n}\right).\end{array}$$

(5)

where $x=M^{3}r/m_{\mathrm{p}}^3{\ell }_{\mathrm{p}}$, $L_{n-1}^1$ are generalised Laguerre polynomials with $n\ge 1$ (the angular momentum is zero) and the corresponding eigenvalues read

$$\begin{array}{c}\hfill \frac{{\mathcal{E}}_n}{M}\simeq -\frac{G_{\mathrm{N}}^2{M}^4}{2{\hslash }^2{n}^2}=-\frac{1}{2n^2}{\left(\frac{M}{m_{\mathrm{p}}}\right)}^4=\frac{1}{2}\left(\frac{E_n^2}{M^2}-1\right).\end{array}$$

(6)

The width of the above eigenstates is given by

$$\begin{array}{c}\hfill R_n\equiv \langle {\Psi }_n\left|R\right|{\Psi }_n\rangle \simeq \frac{{\hslash }^2{n}^2}{G_{\mathrm{N}}{M}^3}=n^2{\ell }_{\mathrm{p}}{\left(\frac{m_{\mathrm{p}}}{M}\right)}^3.\end{array}$$

(7)

In Newtonian physics, there would be no restriction to the spectrum, ${\mathcal{E}}_n$, and, since $R_{n\sim 1}\sim {\ell }_{\mathrm{p}}{(m_{\mathrm{p}}/M)}^3\ll {\ell }_{\mathrm{p}}$, one practically recovers the classical singularity with energy density of the order of $M/R_1^3\sim {(M/m_{\mathrm{p}})}^{9}M{\ell }_{\mathrm{p}}^{-3}$. However, the non-linear relation for $E_n$ in Equation (6) yields the condition

$$\begin{array}{c}\hfill 0\le \frac{E_n^2}{M^2}\simeq 1-\frac{1}{n^2}{\left(\frac{M}{m_{\mathrm{p}}}\right)}^4\Rightarrow n\ge N_M\simeq {\left(\frac{M}{m_{\mathrm{p}}}\right)}^2.\end{array}$$

(8)

The (minimum) quantum number, $N_M$, for the actual ground state, ${\Psi }_{N_M}$, therefore, depends on the mass, M, as required by the quantisation of the horizon area [8] and the corpuscular model of black holes [9,10]. Moreover, ${\Psi }_{N_M}$ has a width

$$\begin{array}{c}\hfill R_{N_M}\sim R_{\mathrm{H}},\end{array}$$

(9)

which grows with M, hence hinting to classicalisation in Einstein gravity [5]. The ground state, ${\Psi }_{N_M}$, could be viewed as a black hole, since $R_{N_M}<R_{\mathrm{H}}$ (see Figure 1 for an example), but we further need to check that the outer geometry is still very close to the Schwarzschild metric (1) to support that conclusion.

3. Quantum Schwarzschild Geometry

We next try and reconstruct the geometry outside the collapsed object. For that purpose, we will use a scalar field $\Phi =V_{\mathrm{N}}/\sqrt{G_{\mathrm{N}}}$ for simplicity [7]. Of course, the field $\Phi$ should not be viewed as fundamental but as a convenient representation of the non-perturbative behaviour of gravity generated by a large compact source.

The important physical assumption is that the quantum gravity vacuum state $|0\rangle$ is the realisation of a universe in which no modes (of matter or gravity) are excited. It is not a priori obvious if it makes any sense at all to associate a Lorentzian metric ${\eta }_{\mu \nu }$ to such an absolute vacuum, but we further notice that this is the metric normally used to describe linearised gravity and to define both matter and gravitational excitations in this regime. The linearised theory should provide a reliable description for small matter sources (say with total energy $M\ll m_{\mathrm{p}}$) and allow one to recover the Newtonian potential from simple tree-level graviton exchanges. Of course, the Newtonian potential is not a fundamental scalar, but it emerges from the (non-propagating) temporal polarisation of virtual gravitons (see, Ref. [11]). For large sources (that is, with $M\gg m_{\mathrm{p}}$), one should reconstruct the proper quantum state from the excitations of the linearised theory, which appears rather hopeless in this highly non-linear regime. In fact, one then usually assumes that there exists a classical background geometry to replace ${\eta }_{\mu \nu }$ with the solution $g_{\mu \nu }$ of the corresponding classical Einstein’s equations. Since we are interested in static and spherically symmetric configurations representing a black hole, we will just require that the quantum state of gravity effectively reproduces (as closely as possible) the expected Schwarzschild geometry (1), which, in turn, contains only one metric function $V_{\mathrm{N}}=V_{\mathrm{N}}\left(r\right)$. We will then see that requiring that $V_{\mathrm{N}}=\sqrt{G_{\mathrm{N}}}\Phi$ emerges from a properly defined quantum state leads to specific restrictions that could not otherwise be unveiled.

For the above reasons, we impose that $\Phi$ satisfies the free massless wave equation in Minkowski spacetime in spherical coordinates,

$$\begin{array}{c}\hfill \left[-\frac{{\partial }^2}{\partial t^2}+\frac{1}{r^2}\frac{\partial }{\partial r}\left(r^2\frac{\partial }{\partial r}\right)\right]\Phi (t,r)=0.\end{array}$$

(10)

Normal modes will then be written in terms of spherical Bessel functions $j_0=sin\left(kr\right)/kr$ as $u_k(t,r)=e^{-ikt}{j}_0\left(kr\right)$. Annihilation operators ${\widehat{a}}_k$ and creation operators ${\widehat{a}}_k^{†}$ for these modes satisfy the usual harmonic oscillator algebra and a Fock space can be built starting from the quantum Minkowski vacuum ${\widehat{a}}_k|0\rangle =0$. We remark once more that this Fock space effectively represents excitations that reduce to temporally polarised gravitons in the linear regime and not the independent (propagating) gravitational degrees of freedom (corresponding to helicity-2 gravitational waves, which should play no role in purely static configurations).

Classical configurations usually emerge in the quantum theory as coherent states. The use of coherent states in quantum field theory to describe static configurations is supported, for instance, by calculations in electrodynamics [12], in Newtonian physics [13] and for the de Sitter spacetime [14,15]. A general coherent state can be written in terms of Fock states as

$$\begin{array}{c}\hfill |g\rangle =e^{-N_{\mathrm{G}}/2}exp\left\{{\int }_0^{\infty }\frac{k^2\mathrm{d}k}{2{\pi }^2}{g}_k{\widehat{a}}_k^{†}\right\}|0\rangle ,\end{array}$$

(11)

and we will then require that

$$\begin{array}{c}\hfill \sqrt{\frac{{\ell }_{\mathrm{p}}}{m_{\mathrm{p}}}}\langle g|\widehat{\Phi }(t,r)|g\rangle =V_{\mathrm{N}}\left(r\right)={\int }_0^{\infty }\frac{k^2\mathrm{d}k}{2{\pi }^2}{\tilde{V}}_{\mathrm{N}}\left(k\right)j_0\left(kr\right),\end{array}$$

(12)

where

$$\begin{array}{c}\hfill V_{\mathrm{N}}=-\frac{G_{\mathrm{N}}M}{r}\end{array}$$

(13)

is the “potential” in the Schwarzschild metric (1). In particular, the occupation numbers for each mode k is found to be given by

$$\begin{array}{c}\hfill g_k=-\frac{4\pi M}{\sqrt{2k^3}{m}_{\mathrm{p}}}.\end{array}$$

(14)

The state $|g\rangle$ is well-defined only if it is normalisable. This condition is tantamount to having a finite total occupation number

$$\begin{array}{c}\hfill N_{\mathrm{G}}={\int }_0^{\infty }\frac{k^2\mathrm{d}k}{2{\pi }^2}{g}_k^2=4\frac{M^2}{m_{\mathrm{p}}^2}{\int }_0^{\infty }\frac{\mathrm{d}k}{k}.\end{array}$$

(15)

However, this integral diverges both in the infrared (IR) and the ultraviolet (UV), and no coherent quantum state exists in our Fock space, which can reproduce the classical potential in Equation (13) exactly.

The actual occupation numbers $g_k$ for $k\to 0$ and $k\to \infty$ could be determined if we had a complete quantum theory of gravity, but here we will just consider generic behaviours that regularise the expression (15). In particular, the IR divergence stems from the assumption of exact staticity, which lets the potential $V_{\mathrm{N}}$ extend to infinity. We can then introduce a cut-off $k_{\mathrm{IR}}=1/\tau$ as a formal way to account for the finite lifetime $\tau$ of a real source. The UV divergence would not be present if the source had finite size and, from the description of collapsed matter inside black holes in the previous section, we simply introduce a cut-off $k_{\mathrm{UV}}\sim 1/R_{N_M}\sim 1/M$. This again yields the horizon area quantisation [8], that is

$$\begin{array}{c}\hfill N_{\mathrm{G}}=4\frac{M^2}{m_{\mathrm{p}}^2}{\int }_{k_{\mathrm{IR}}}^{k_{\mathrm{UV}}}\frac{\mathrm{d}k}{k}\simeq 4\frac{M^2}{m_{\mathrm{p}}^2}ln\left(\frac{\tau }{G_{\mathrm{N}}M}\right),\end{array}$$

(16)

in which the logarithm appears because of the choice of a sharp UV cut-off and would be replaced with a more accurate description of the matter source. We also notice that the average radial momentum is given by

$$\begin{array}{c}\hfill \langle k\rangle =4\frac{M^2}{m_{\mathrm{p}}^2}{\int }_{k_{\mathrm{IR}}}^{k_{\mathrm{UV}}}\mathrm{d}k=4\frac{M^2}{m_{\mathrm{p}}^2}\left(\frac{1}{G_{\mathrm{N}}M}-\frac{1}{\tau }\right),\end{array}$$

(17)

so that both M and the typical wavelength ${\lambda }_{\mathrm{G}}=N_{\mathrm{G}}/\langle k\rangle \sim {\ell }_{\mathrm{p}}M/m_{\mathrm{p}}$ reproduce the scaling laws of the corpuscular model of black holes [9].

Having defined a proper quantum state $|g\rangle$, we can next obtain the corresponding geometry by replacing $V_{\mathrm{N}}$ in Equation (1) with

$$\begin{array}{c}\hfill V_{\mathrm{QN}}\simeq {\int }_{k_{\mathrm{IR}}}^{k_{\mathrm{UV}}}\frac{k^2\mathrm{d}k}{2{\pi }^2}{\tilde{V}}_{\mathrm{N}}\left(k\right)j_0\left(kr\right)\simeq V_{\mathrm{N}}\left\{1-\left[1-\frac{2}{\pi }\mathrm{Si}\left(\frac{r}{G_{\mathrm{N}}M}\right)\right]\right\},\end{array}$$

(18)

where $\mathrm{Si}$ is the sine integral function. The quantum corrected metric still contains a horizon (see Figure 2 for an example) but the Ricci scalar $\mathcal{R}\sim r^{-2}$ and the Kretschmann scalar ${\mathcal{R}}_{\alpha \beta \mu \nu }{\mathcal{R}}^{\alpha \beta \mu \nu }\sim {\mathcal{R}}^2\sim r^{-4}$, for $r\to 0$, whereas the Kretschmann scalar in the classical Schwarzschild spacetime diverges as $r^{-6}$. This ensures that tidal forces remain finite at the centre, as can be seen more explicitly from the relative acceleration of radial geodesics for $r\to 0$ (In the Schwarzschild spacetime $a\sim r^{-4}$; thus, causing the “spaghettification” of infalling matter),

$$\begin{array}{c}\hfill a\equiv \frac{\ddot{\Delta r}}{\Delta r}=-{\mathcal{R}}_{010}^1\simeq \frac{G_{\mathrm{N}}^2{M}^2}{R_{\mathrm{s}}^4},\end{array}$$

(19)

where $\Delta r$ is the separation between two nearby radial geodesics. One can further compute the effective energy-momentum tensor ${\mathcal{T}}_{\mu \nu }$ from the Einstein tensor $G_{\mu \nu }$ of the metric (18) and find that the effective energy density $\rho \simeq -G_0^0\sim r^{-2}$, with the effective radial pressure $p_r\simeq G_1^1=-\rho \sim r^{-2}$ and the effective tension $p_t\simeq G_2^2\sim r^{-2}$. The integral of these quantities over space, therefore, remains finite and the point $r=0$ is said to be an integrable singularity. Moreover, there is no second horizon, and the spacetime is not affected by any of the issues associated with inner Cauchy horizons. From the phenomenological point of view, it is important that the oscillations shown in Figure 2 occur around the expected classical behaviour $V_{\mathrm{N}}$ and become smaller and smaller for decreasing values of $R_{N_M}$ in the region $r>R_{\mathrm{H}}$ (we have just considered $R_{N_M}=G_{\mathrm{N}}M$ here for the sake of simplicity).

4. Conclusions

We briefly reviewed the quantum analyses from Refs. [3,7] for collapsing objects and black holes. We can summarise the main results by saying that (i) matter-forming black holes do not end in a singularity but will reach a final configuration of macroscopic size (much above the Planck length); (ii) the corresponding effective metric is regular everywhere, including the centre, and contains information about (at least) the size of the material core, which constitutes a form of quantum hair [16]; and (iii) both the quantum ground state of the collapsed matter and the quantum state of the outer geometry are characterised by similar scalings of the mass $M^2\sim N_M\sim N_{\mathrm{G}}$, from Equations (8) and (16). The above picture is thus compatible with the quantisation of the horizon area [8], the idea that gravity classizalises at large energies [5], and the corpuscular picture of black holes [9].