Abstract
We study the fluctuations and the correlations between spatial regions generated in the primordial quantum gravitational era of the universe. We point out that these can be computed using the Lorentzian dynamics defined by the Loop Quantum Gravity amplitudes. We evaluate these amplitudes numerically in the deep quantum regime. Surprisingly, we find large fluctuations and strong correlations, although not maximal. This suggests the possibility that early quantum gravity effects might be sufficient to account for structure formation and solve the cosmological horizon problem.
1 Introduction
Standard cosmology–with or without inflation–requires an initial state that exhibits fluctuations and correlations between distinct regions of space. These play a key role, in particular as seeds for structure formation. Here we investigate how these fluctuations and correlations can emerge from a primordial quantum gravitational cosmological phase, using Loop Quantum Gravity (LQG) and a simple model of the early universe.
We consider the quantum transition from an empty state to a 3-geometry. The amplitude of this transition may be relevant in a Big Bang cosmology (; ; ), as well as in a bouncing cosmology, where it dominates the transition through the bounce (; Vidotto, 2011; ). We treat the dynamics of gravity non-perturbatively, using covariant LQG. This calculation does not require a Wick rotation and it is well defined in the Lorentzian theory. The transition generates a quantum state that defines the probability distribution over 3-geometries. This includes correlations between spatially separated regions.
We truncate the degrees of freedom of the gravitational field to a small finite number in addition to the scale factor [cfr (; ; Vidotto, 2017)]. Using numerical methods, we obtain four results: 1) The expectation value of the geometric variables at a given value of the scale factor yields precisely (the truncation of) a metric 3-sphere. 2) Contrary to our initial expectation, the variance of these variables is very large: the amplitude of the fluctuations is significant. 3) Correlations between variables in distinct regions–and entanglement entropy between regions–do not vanish with the increase of the scale factor. 4) Entanglement entropy appears to converge to a stable value asymptotically.
All this indicates that the universe emerging from an early quantum era includes fluctuations, homogeneity properties, and large scale correlations, due to the common quantum origin of spatially separated regions. These can be studied theoretically and appear to be compatible with the observed universe. In particular, inflation or a bounce might not be strictly necessary to circumvent the horizon problem. If the initial quantum phase is taken into account, our result suggests that distant regions may have not been causally disconnected in the past, as in classical cosmology.
2 Quantum Theory
We discretize a closed cosmological 3-geometry into five tetrahedra glued to one another, giving an S3 topology. This is a regular triangulation of a topological 3-sphere, and it corresponds to the boundary of a 4-simplex. The geometry of a flat 4-simplex has twenty degrees of freedom, which capture the gravitational field in this truncation. The result of the transition from nothing to a 3-geometry is described by its covariant LQG Lorentzian amplitude (Vidotto, 2011). The truncation we consider corresponds to the single vertex amplitude, to the first order in the spinfoam expansion (). We take the areas of the faces of the tetrahedra to be equal and use this common value as a proxy for the physical scale factor. The remaining degrees of freedom characterize the shapes of the five tetrahedra. We are interested in the fluctuations of these variables and the correlations between variables in distinct tetrahedra, at different values of the scale factor.
The LQG Hilbert space for this truncation is , where is the complete graph with five nodes. See () for the notation and an introduction to the formalism. We label the (oriented) links as , or alternatively in terms of the two nodes they link: . The spin network basis in is given by the states where the jl’s are spins (half-integer values labeling irreps) and the in’s are a basis in the corresponding intertwiner space , where Vj is the spin-j representation space of . We focus on the subspaces of defined by . These have the tensorial structure , where each is isomorphic to . The basis states are tensor states, which we denote as (by this we mean ). We choose a basis in fixing a pairing of the links at each node and the basis that diagonalizes the modulus square of the sum of the generators in the pair.
The transition amplitude from an empty state to a state in is given by the spinfoam amplitude of the boundary state alone. This is because this transition corresponds to the amplitude of a boundary state that has only one connected component, here interpreted as the future one. To first order in the spinfoam expansion, the amplitude of a boundary state is given by a single vertex. Hence the nothing-to- amplitude is the vertex amplitude for the boundary statewhere is the Lorentzian EPRL vertex amplitude (). This implies that we can view the ket with components , as the quantum state emerging from the Big Bang. This is the analogue, in (Lorentzian) LQG, of the Hartle-Hawking “no-boundary” initial state in (Euclidean) path-integral quantum gravity (). This is the state we are interested in. We study the mean geometry it defines and the quantum fluctuations and correlations it incorporates. Specifically, we study the expectation value , the spread and the (normalized) correlationsof local geometry operators defined on . We compute also the entanglement entropy of a node with respect to the rest of the graph, where is the reduced density matrix of the state at any node, all nodes being equivalent by symmetry.
3 Quantum Geometry
The spin-network basis states can be viewed as a collection of quantum tetrahedra () glued together by identifying faces. Shared faces have the same area but not necessarily matching shapes, giving rise to a twisted geometry (). The areas of the faces are eigenvalues of the area operatorwritten in terms of the flux operatorsentering the node n on link l, where γ is the Barbero-Immirzi constant and is the vector of generators on link l. The shape of the tetrahedron is measured by the angle operatorthat gives the cosine of the external dihedral angle between faces a and b, where
Say we use the recoupling basis that pairs links and at node n, and let be the intertwiner state at node n. The operator is diagonal on with eigenvaluewhere is the intertwiner spin. Putting together Eqs 3, 5, and 6 we obtainfor measuring the dihedral angle of in terms of intertwiner spin .
4 Numerical Methods
The Lorentzian EPRL vertex amplitude can be written as where f and e label the faces and the half-edges touching the vertex. The symbol is the invariant symbol built from contracting the five 4-valent intertwiners at the nodes, and can be expressed as the contraction of five symbols asThe functions are defined aswhere the factors in front of the integral are symbols and the functions are boost matrix elements of the Lorentz group. The product in Eq. 8 is over four of the five half-edges because one redundant factor must be eliminated by gauge-fixing. The sum is over a set of auxiliary spins and auxiliary intertwiners . See for more details about this formulation of the EPRL amplitude and the full definition and analysis of all the quantities involved in the previous formulae.
Analytical results show that in the large spin limit this amplitude is generally exponentially suppressed except in two cases (; ). The first case is when the boundary geometry is the geometry of the boundary of a Lorentzian 4-simplex. This case can be naturally related to the semiclassical limit, where spacetime is flat and Lorentzian at scales smaller than the curvature radius. The second case is when the boundary geometry is a vector geometry, which includes the case when the boundary geometry is the geometry of the boundary of a Euclidean 4-simplex. As we shall see below, the mean geometry defined by is that of a discretized metric 3-sphere i.e., the boundary of a regular Euclidean 4-simplex. Therefore this is a vector geometry. Vector geometries have been considered as a puzzling feature of the theory (): here we can interpret them as a necessary contribution to the primordial quantum cosmological state in order to allow the tunneling from the empty state to the semiclassical 3-sphere geometry.
The form of the amplitude Eq. 8 is suited for numerical evaluation. The computational steps, in order of increasing complexity and cost, are: 1) evaluation of the symbol; 2) evaluation of the B functions and 3) contraction over all internal and boundary spin labels. We limited our computation to spins (i.e., scale factor) given the time and memory constraints imposed by our computing facility. We used a standard laptop computer for lower spins and a 32-cores server with 196 GBs of RAM for higher spins.
The sum over spins in Eq. 8 is unconstrained, as , where link l corresponds to face f. Hence it is necessary to introduce a cutoff so that and the exact value is in the limit . The case with has been called the simplified model (). Since the computation time is proportional to , we are limited to very low values of the cutoff. It can be shown that in the simplified model the Lorentzian part of the amplitude is partially suppressed (; ), and the effect of increasing the cutoff is to gradually enhance the amplitude for Lorentzian configurations. It may seem necessary to reach higher cutoffs in order to match the expected behavior in semiclassical asymptotics of Lorentzian simplices (). However, we found that in our calculation, which spans the space of vector geometries due to the chosen (Euclidean) boundary conditions, the corrections due to higher cutoff values are minor or even negligible, so that the simplified computations effectively suffice to study the model numerically.
All the computations of the present work were carried out using the sl2cfoam library (), which is a C library for computing the spinfoam amplitude Eq. 8 using various optimization strategies. For a complete treatize of all the technical and numerical details that are relevant to this work we refer also to (Gozzetti, 20211), which studies extensions of the model considered here using a recently released version of the library (Gozzetti, 20212).
5 Numerical Results
The results below are given for increasing values of the scale parameter
j. In this section we fix the cutoff parameter to
. Therefore from now on we fix the convenient values
and the Barbero-Immirzi constant to
.
1.The expectation value of the angle operator that measures the external dihedral angles between faces punctured by links a and b in any of the boundary tetrahedra (by symmetry all of them are equivalent) results to be
which is precisely the cosine of the external dihedral angle of an equilateral tetrahedron, for any links
chosen. This shows that the spatial metric of
averages to that of the 3-boundary of a regular 4-simplex i.e., to that of a 3-sphere in our approximation. The variation of the average with the scale parameter is minor and due entirely to numerical fluctuations (
Figure 1). The independence of the result from the choice of the links was tested by switching to a different recoupling basis, and also by directly performing the change of basis.
1.The spread is large and increasing with the scale factor, see Figure 2. This suggest that quantum fluctuations in the metric are wide and are not suppressed in the large-scale regime.
2.The correlations between angle operators on different nodes depend on the pairing. We write for the angle operator at node n, where link a connects n with and link b connects n with . The correlations are shown in Figure 3. For each source node n there are two pairs of correlated—anti-correlated nodes (for these are and ). The correlations appear to reach an asymptotic value, hence are not suppressed in the large-scale regime. The 3-metric that comes out from the quantum state can correlate different spatial patches of the primordial universe, as required for solving the horizon problem of standard cosmology. It would be interesting to verify that in finer triangulations the correlations decay with the distance between non-adjacent faces, as required by local effective field theory.
3.To quantify the degree of correlation between operators we computed the entanglement entropy between different tetrahedra, viewed as quantum subsystems. A result by Page () states that, given a splitting of a Hilbert space into subspaces corresponding to a small subsystem R and its complement , the typical state in is found to have an entanglement entropy equal to corresponding to a maximally-mixed state. In other words, the vast majority of quantum states of a small subsystem are close to being, in a broad sense, thermal see .
FIGURE 1
FIGURE 2
FIGURE 3
We studied the degree of non-typicality of the primordial state by looking at the entanglement entropy of any tetrahedron as function of the scale factor. The result is shown in Figure 4. It indicates that the entropy deviates significantly from the maximally-mixed case, and it appears to get close to an asymptotic value in the limit of large scale factor. We could not push the computations to spins higher than , but the qualitative behavior is clear. For comparison, we show also the maximum entropy and the result of () on the so-called Bell-network states (), which are constructed in the same way as our primordial state but using the dynamics of the simpler BF theory. See also (; ).
FIGURE 4
6 Conclusion
Summarizing, the quantum state for the primordial universe predicted by the dynamics of Loop Quantum Gravity can be computed in a kinematical truncation and at first order in the vertex expansion. It describes the fluctuating metric of a topologically closed universe in its early quantum regime. Its degrees of freedom encode the shapes of neighboring spatial regions. Their size (area), taken to be equal, is related to the scale factor. We have found that the mean geometry of this state is that of a (truncated) 3-sphere, as we expected by symmetry, but the fluctuations are large. Neighboring regions are correlated and correlations do not vanish as the scale factor increases. This opens the possibility that an inflationary phase may not be needed in order to circumvent the horizon problem, as the primordial quantum phase may introduce stochastic correlations in otherwise causally-independent spatial regions. We also computed the entanglement entropy of a single region viewed as a quantum subsystem of the whole universe. We found that the cosmological state is highly non-typical, showing an entanglement entropy that is apparently reaching an asymptotic value as the scale factor increases. Our work is one of the first explorations of the purely quantum regime of LQG—without resorting to the high-spin semiclassical limit of the theory—and one of the first applications to a concrete physical model of the numerical tools that are recently being developed for covariant Loop Quantum Gravity (; ; ; ). Our results indicate that an early quantum phase of the universe may provide an explanation for known puzzling features of the standard cosmological model, such as the horizon problem, possibly even without introducing additional inflationary and/or bouncing phases.
We thank for discussions Pietro Doná, Carlo Rovelli, Giorgio Sarno and Simone Speziale. We thank the Department of Theoretical Physics at UPV/EHU where part of this research was carried, supported by the grant IT956-16 of the Basque Government and by the grant FIS2017-85076-P (MINECO/AEI/FEDER, UE). We acknowledge the Anishinaabek, Haudenosaunee, Lūnaapéewak, and Attawandaron peoples, on whose traditional lands Western University is located.
Statements
Data availability statement
The raw data supporting the conclusion of this article will be made available upon request by the authors, without undue reservation.
Author contributions
FG contributed to this work writing an original code, performing all the numerical computations, and contributing to the analytical aspects of the computation. FV contributed with the original idea of this paper, devising the computations, supervising their completions, and analysing the results.
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.
Footnotes
1.^Gozzini (2021). High performance lorentzian spin foam numerics. In preparation.
2.^Gozzini (2021). Numerical simulation of the quantum cosmological vacuum with many spin foam vertices. In preparation.
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Summary
Keywords
quantum gravity, cosmology, structure formation, spinfoam, spinfoam cosmology, horizon problem, loop quantum gravity
Citation
Gozzini F and Vidotto F (2021) Primordial Fluctuations From Quantum Gravity. Front. Astron. Space Sci. 7:629466. doi: 10.3389/fspas.2020.629466
Received
14 November 2020
Accepted
28 December 2020
Published
18 February 2021
Volume
7 - 2020
Edited by
Antonino Marciano, Fudan University, China
Reviewed by
Sayantan Choudhury, National Institute of Science Education and Research, India
Vyacheslav Ivanovich Dokuchaev, Institute for Nuclear Research, Russia
Updates
Copyright
© 2021 Gozzini and Vidotto.
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: Francesca Vidotto, fvidotto@uwo.ca
This article was submitted to Cosmology, a section of the journal Frontiers in Astronomy and Space Sciences
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