Printer Friendly

Big Bang as a Critical Point.

1. Introduction

Accumulating results of theoretical investigations indicate that the gravitational field exists in different phases. First indications supporting such an idea came from considerations of three-dimensional Euclidean quantum gravity [1]. By means of Monte Carlo simulations it was possible to explore the configuration of the gravitational field under various conditions. For four-dimensional Euclidean gravity, gravity exhibits two phases: the crumpled phase and the branched polymer phase [2]. This result has since been generalized to the case of four-dimensional gravity with an imposed causality condition, formulation known as Causal Dynamical Triangulations (CDT). The causality condition turned out to be essential for the correct phase structure of gravity, leading to emergence of the four-dimensional space-time [3]. Generation of such extended phase in the Euclidean approach introducing a nontrivial path integral measure remains an interesting possibility [4]. Furthermore, similarly to a phase structure of the Lifshitz scalar [5], the critical surface of CDT has been divided into three regions separated by the first- and second-order transition lines [6]. Interestingly, a theory describing gravity at a triple point (Lifshitz point) of the phase diagram has been constructed and shown to be power-counting renormalizable [7]. Further evidence for the nontrivial phase structure of gravity comes from Quantum Graphity [8]. This approach utilizes the idea of geometrogenesis: a transition between geometric and nongeometric phases of gravity.

The basic question one can ask, assuming the existence of the different phases of gravity, is where can the other phases be found? A natural place to search for them is high curvature regions such as interiors of the black holes and the early universe. Because of a horizon, a possibility of relating phase change inside of black holes with astronomical observations is a difficult task. Nevertheless, gravitational phase transitions occurring under the black hole horizon, including the signature change transition, have been a subject of theoretical studies (see, e.g., [9, 10]). Perhaps empirically more promising is a search for signatures of the gravitational phase transitions which took place in the early universe. We will focus on this direction here.

So far, there has been very little attention devoted to this issue in the literature. Most studies of the phase transitions in the early universe were dedicated to the matter sector, rather than gravity [11, 12]. Among the few studies on the gravitational phase transitions in the early universe, the work of [13, 14] is especially noteworthy. In [13] a specific model of geometrogenesis, through a second-order phase transition, has been proposed. It was shown that, by assuming the holographic principle to be fulfilled in the high temperature phase, it is possible to generate a power spectrum of primordial perturbations that is in agreement with observations. In [14] the cosmological relevance of second-order phase transitions is discussed. Arguments supporting generation of "inflationary" power spectrum from critical behavior of the gravitational field have been presented.

In what follows we attract attention to the fact that a second-order gravitational phase transition has recently been observed within Causal Dynamical Triangulations [15]. The transition takes place exactly between the phases of the form discussed in [8, 13]. Therefore, CDT gives a concrete realization of the scenario of geometrogenesis. We also show that gravitational phase transition maybe associated with the deformation of general covariance, recently observed in the context of Loop Quantum Cosmology (LQC). In both cases, the phase transition is of second order, suggesting a critical nature of the emergence of classical space-time in the early universe.

2. Causal Dynamical Triangulations

Analysis performed within four-dimensional CDT with a positive cosmological constant indicates the presence of three different phases of the gravitational field, called A, B, and C [6]. The phases are separated by the first- (A-C) and second-order (B-C) transition lines presumably intersecting at the triple point. The order of the A-B phase transition has not been determined so far.

At large scales, phase C forms the four-dimensional de Sitter space [16]. The phase is, however, not fully classical since it exhibits dimensional reduction to two dimensions at short scales [17]. This can be shown by investigating properties of the spectral dimension, defined via a diffusion process. Nevertheless, the phase C can be associated with the "usual" phase of gravity. The two remaining phases are fundamentally different from this phase. Phase A is characterized by a vanishing interaction between adjacent time slices. Phase B, resembling the crumpled phase in Euclidean gravity, is characterized by a large (tending to infinity in the [infinity]- volume limit) Hausdorff and spectral dimension. Phase B shares features of the high temperature phase postulated in Quantum Graphity. Moreover, this phase is separated with the low energetic phase C by the second-order phase transition. This is in one-to-one correspondence to the Quantum Graphity case. Based on this observation, we hypothesize the following.

Hypothesis 1. In the early universe, there was a second- (or higher) order phase transition from the high temperature nongeometric phase to the low temperature geometric phase of gravity. The transition is associated with a change of the connectivity structure between the elementary chunks of space.

The change of connectivity can be inferred from the considerations of the spectral dimensions of the phases B and C. In order to see it explicitly let us consider a toy model of the universe composed of the N chunks of space. They will be represented by the nodes of a graph. A structure of adjacency is represented by the links.

In phase C, which is a geometric phase, the degree of vertices is low. In our toy model it equals 2 and the resulting space is represented by the Ring graph (see Figure 1(a)). The spectral dimension of this graph can be found by determining spectrum (eigenvalues [X.sub.n]) of the Laplace operator [DELTA] = A - D, where A is an adjacency matrix and D is a degree matrix. By using the expression for the trace of the heat kernel K one can find that

[mathematical expression not reproducible], (1)

where [sigma] is a diffusion time.

In Figure 2 we plot function (1) for the Ring graph, for which the eigenvalues are [[lambda].sub.n] = 2(cos(2[pi]n/N) - 1). At intermediate diffusion times the spectral dimension is equal to one, as expected classically. The short time behavior, corresponding to dimensional reduction observed in the four-dimensional case, is due to the discrete nature of the network. Furthermore, at large diffusion times the spectral dimension is again falling to zero due to the compactness of space (not visible in Figure 2).

Let us now model the high temperature nongeometric phase B by assuming, for computational simplicity, a maximal degree of nodes. The resulting Complete graph is shown in Figure 1. The assumption of completeness allows one to determine spectrum of the Laplace operator analytically and enables the simplification of (1) to

[d.sub.S] = 2N[sigma](N - 1)/[e.sup.N[sigma]] + (N - 1). (2)

We plot this function in Figure 2, comparing it with the low temperature case. As we see, the spectral dimension is now peaked at small diffusion times. The maximal value of the spectral dimension grows with the number of nodes as [d.sub.S,max] [approximately equal to] 2W(N/e), where W(x) is the Lambert function. This behavior is in qualitative agreement with the numerical computations performed in four-dimensional CDT [6].

3. Loop Quantum Cosmology

Recent developments in LQC indicate that the hypersurface deformation algebra (HDA) is deformed due to the quantum gravitational effects [18]. This means that the general covariance is quantum deformed, but not broken.

In condensed matter physics, a change of symmetry is often associated with the occurrence of a phase transition. By extrapolating this observation to the sector of gravitational interactions, we make the following hypothesis.

Hypothesis 2. Phases of gravity are distinguished by different types of hypersurface deformation algebras.

In order to support this hypothesis we present an example based on holonomy corrections in LQC. In this case, HDA is deformed such that {S, S} = [OMEGA]D, where S are scalar constraints and D is a diffeomorphism constraint, and the remaining brackets are unchanged [19]. The [OMEGA] = l-2([rho]/[[rho].sub.c]) is a deformation factor, p denotes energy density of matter, and [[rho].sub.c] is a maximal energy density expected to be of the order of the Planck energy density.

At low energy densities, the classical Lorentzian HDA with [OMEGA] = 1 is recovered, while at [rho] = [[rho].sub.c], [OMEGA] = -1 corresponding to Euclidean space. Approaching the Planck epoch is therefore associated with the signature change from Lorentzian space-time to Euclidean four-dimensional space [20]. Interestingly, at [rho] = [[rho].sub.c]/2 the HDA reduces to the ultralocal form ({S, S} = 0) describing a state of silence [21]. This state shares properties of phase B in CDT, giving a first indication for the relationship between the phase of gravity and deformation of HDA. This is, in particular, because the ultralocal limit is characterized by collapse of light-cones (c [right arrow] 0). In CDT, the length of time links becomes dominant over the length of the spatial links while approaching the B phase, which can be interpreted as an effective decrease of the speed of light. Furthermore, in the B phase the space points collapse into the crumpled configuration with no spatial extension. Such behavior is in agreement with properties of the ultralocal limit. Therefore, one can presume that the geometrogenesis related to the second-order phase transition from phase B to phase C is associated with the change of the HDA from the ultralocal one ({S, S} = 0) to the one characterizing classical gravity ({S, S} = D). The phase change is, therefore, reflected by an appropriate change of symmetry, which is embedded in the form of HDA. Surprisingly, the deformation of HDA observed in LQC (i.e., {S, S} = [OMEGA]D) continuously interpolates between the ultralocal and geometric phases.

Worth stressing is that besides the classical limits with either [OMEGA] = 1 (Lorentzian manifold) or [OMEGA] = -1 (Euclidean manifold), the geometry associated with the deformed HDA is poorly understood. It is known that the deformed algebra leads to gauge transformations which do not commute with the Lie derivatives. This indicates that the standard notion of an invariant metric has to be generalized appropriately and the geometry has non-Riemannian character [22]. This concerns both the deformations observed in the cosmological sector (LQC) as well in the spherical symmetric case. Nevertheless, even if the standard metric loses its meaning in the intermediate regime, Hamiltonian dynamics remains well defined and the structure of causality can be inferred based on analysis of equations of motions and the corresponding characteristic equations (see [23]). This, in particular, concerns the ultralocal state which interpolates between the regions of negative and positive values of the deformation factor [OMEGA].

Further evidence supporting Hypothesis 2 comes from a simple model of the signature change as a spontaneous symmetry breaking (SBB) associated with a second-order phase transition [23]. The symmetry breaking is from SO(4) to SO(3) at the level of an effective homogeneous vector field [[phi].sub.[mu]] . This translates to a symmetry change from SO(4) to SO(3,1), experienced by the field living on a geometry described by the metric [g.sub.[mu]v] = [[delta].sub.[mu]v] - 2[[phi].sub.[mu]][[phi].sub.v].

Let us assume that the free energy for the model with a massless scalar field v is

[mathematical expression not reproducible], (3)

where [absolute value of ([??])] = [square root of ([[delta].sup.[mu]v][[phi].sub.[mu]][[phi].sub.v])] and [beta] is a constant. Due to the symmetry breaking kinetic factor, the expression for the free energy is not explicitly SO(4) invariant. Treating this term as a perturbation (which is valid for sufficiently small values of v), the equilibrium is obtained by minimizing value of the potential

At energy densities [rho] > [[rho].sub.c] the vacuum state maintains the SO(4) symmetry, leading to [absolute value of ([??])] = 0. The metric elements are therefore [g.sub.00] = 1 and [g.sub.ii] = 1, representing the four-dimensional Euclidean space. This region is, however, forbidden due to the constraint [rho] [less than or equal to] [[rho].sub.c] present in LQC. In turn, below the critical energy [rho] [less than or equal to] [[rho].sub.c], the minimum of the potential is located at [absolute value of ([??])] = [square root of (1 - [rho]/[[rho].sub.c])] in some spontaneously chosen direction (see Figure 3). Without loss of generality, let us assume that the SSB takes place in direction [[phi].sub.0], for which

[g.sub.00] = 1 - 2[[phi].sub.0][[phi].sub.0] = 1 - 2 (1 [rho]/[[rho].sub.c]) = - 1 + 2 [rho]/[[rho].sub.c] = -[OMEGA], [g.sub.ii] = 1, (4)

leading to the effective speed of light [c.sup.2.sub.eff] = [OMEGA]. As a consequence, the equation of motion for the scalar field v takes the form

[g.sup.[mu]v] [[partial derivative].sub.[mu]][[partial derivative].sub.v]v = - 1/[c.sup.2.sub.eff] [[partial derivative].sup.2]/[partial derivative][t.sup.2]v + [DELTA]v = 0, (5)

manifesting SO(4) symmetry at the critical point ([OMEGA] = -1) and SO(3,1) symmetry in the low temperature limit ([OMEGA] = 1). The form of (5) agrees with the one derived from the holonomy deformations of the HDA [18].

In LQC, energy densities above [[rho].sub.c] cannot be reached. Therefore, the evolution starts at the critical point located at [[rho].sub.c]. An interesting possibility is that the system has been maintained at the critical point before the energy density started to drop. This may not require a fine-tuning if the dynamics of the system exhibited Self-Organized Criticality (SOC) [24], which is observed in various complex systems. Interestingly, this concept has already been applied to quantum gravity, however, in order to describe classical configuration of space [25]. Furthermore, it is possible that the region [rho] > [[rho].sub.c] is described by a nongeometric phase of gravity, whose properties cannot be captured within the presented model.

4. Conclusions

We have shown that CDT offers a concrete realization of geometrogenesis, having a second-order gravitational phase transition between the nongeometric and geometric phase. We have explained how measurements of the spectral dimension are related in this case with connectivity of the chunks of space. The critical nature of the emergence of classical space-time in the early universe may give a first possibility of testing CDT. However, this would require more detailed investigations of the properties of the second-order phase transition in CDT. In LQC, which is an alternative to CDT, a gravitational second-order phase transition may explain a signature change in the Planck epoch. In the presented toy model, the universe originates just at the critical point. Furthermore, we have indicated that the phase transition from the nongeometric phase B in CDT to the phase C can be reflected by the deformation of the hypersurface deformation algebra observed in LQC. Interestingly, the latest results in CDT indicate the existence of a new subphase of the phase C [26], characterized by a "bifurcation" of the kinetic term. This behavior resembles the signature change observed in LQC.

https://doi.org/10.1155/2017/4015145

Conflicts of Interest

The author declares that they have no conflicts of interest.

Acknowledgments

Jakub Mielczarek is supported by the National Centre of Science (Grant DEC-2014/13/D/ST2/01895).

References

[1] J. Ambjorn, D. V Boulatov, A. Krzywicki, and S. Varsted, "The vacuum in three-dimensional simplicial quantum gravity," Physics Letters. B. Particle Physics, Nuclear Physics and Cosmology, vol. 276, no. 4, pp. 432-436, 1992.

[2] J. Ambjorn and J. Jurkiewicz, "Four-dimensional simplicial quantum gravity," Physics Letters. B. Particle Physics, Nuclear Physics and Cosmology, vol. 278, no. 1-2, pp. 42-50, 1992.

[3] J. Ambjorn, J. Jurkiewicz, and R. Loll, "Emergence of a 4D world from causal quantum gravity," Physical Review Letters, vol. 93, no. 13, 131301, 4 pages, 2004.

[4] J. Laiho and D. Coumbe, "Evidence for Asymptotic Safety from Lattice Quantum Gravity," Physical Review Letters, vol. 107, no. 16, Article ID 161301, 2011.

[5] R. M. Hornreich, M. Luban, and S. Shtrikman, "Critical behavior at the onset of k[right arrow]-space instability on the X line," Physical Review Letters, vol. 35, no. 25, pp. 1678-1681, 1975.

[6] J. Ambjorn, S. Jordan, J. Jurkiewicz, and R. Loll, Physical Review D, vol. 85, Article ID 124044, 2012, https://journals.aps.org/prd/ abstract/10.1103/PhysRevD.85.124044.

[7] P. Horava, "Quantum gravity at a Lifshitzpoint," Physical Review D, vol. 79, no. 8, Article ID 084008, 2009.

[8] T. Konopka, F. Markopoulou, and L. Smolin, https://arxiv.org/ abs/hep-th/0611197.

[9] G. J. Stephens and B. L. Hu, "Notes on black hole phase transitions," International Journal of Theoretical Physics, vol. 40, no. 12, pp. 2183-2200, 2001.

[10] M. Bojowald, S. Brahma, and J. D. Reyes, "Covariance in models of loop quantum gravity: spherical symmetry," Physical Review D: Covering Particles, Fields, Gravitation, and Cosmology, vol. 92, no. 4, Article ID 045043, 2015.

[11] T. W. B. Kibble, "Topology of cosmic domains and strings," Journal of Physics A: Mathematical and General, vol. 9, no. 8, 1974.

[12] W. H. Zurek, "Cosmological experiments in superfluid helium?" Nature, vol. 317, no. 6037, pp. 505-508, 1985.

[13] J. Magueijo, L. Smolin, and C. R. Contaldi, "Holography and the scale invariance of density fluctuations," Classical and Quantum Gravity, vol. 24, no. 14, pp. 3691-3699, 2007.

[14] O. Dreyer, "The world is discrete," https://arxiv.org/abs/ 1307.6169.

[15] J. Ambjorn, S. Jordan, J. Jurkiewicz, and R. Loll, "Second-order phase transition in causal dynamical triangulations," Physical Review Letters, vol. 107, Article ID 211303, 2011, https:// journals.aps.org/prl/abstract/10.1103/PhysRevLett.107.211303.

[16] J. Ambjorn, A. G, J. Jurkiewicz, R. Loll, and A. Gorlich, "Planckian Birth of a Quantum de Sitter Universe," Physical Review Letters, vol. 100, Article ID 091304, 2008, https://journals.aps.org/ prl/abstract/10.1103/PhysRevLett.100.091304.

[17] J. Ambjorn, J. Jurkiewicz, and R. Loll, "The Spectral Dimension of the Universe is Scale Dependent," Physical Review Letters, vol. 95, Article ID 171301, 2005, https://journals.aps.org/prl/ abstract/10.1103/PhysRevLett.95.171301.

[18] M. Bojowald and G. M. Paily, "Deformed general relativity and effective actions from loop quantum gravity," Physical Review D, vol. 86, Article ID 104018, 2012, https://journals.aps.org/prd/ abstract/10.1103/PhysRevD.86.104018.

[19] T. Cailleteau, J. Mielczarek, A. Barrau, and J. Grain, "Anomaly-free scalar perturbations with holonomy corrections in loop quantum cosmology," Classical and Quantum Gravity, vol. 29, no. 9, Article ID 095010, 17 pages, 2012.

[20] J. Mielczarek, "Signature change in loop quantum cosmology," General Relativity and Quantum Cosmology, p. gr, 2014, https://arxiv.org/abs/1207.4657.

[21] J. Mielczarek, "Asymptotic silence in loop quantum cosmology," AIP Conference Proceedings, vol. 1514, no. 1, 2013, http://aip.scitation.org/doi/abs/10.1063/1.4791730.

[22] M. Bojowald, S. Brahma, U. Buyukcam, F. DAmbrosio, and D. Phys. Rev, "Hypersurface-deformation algebroids and effective spacetime models," Physical Review D, vol. 94, no. 10, Article ID 104032, 2016, https://journals.aps.org/prd/ abstract/10.1103/PhysRevD.94.104032.

[23] M. Bojowald and J. Mielczarek, "Some implications of signature-change in cosmological models of loop quantum gravitys," Journal of Cosmology and Astroparticle Physics, vol. 2015, 2015, http://iopscience.iop.org/article/10.1088/1475-7516/ 2015/08/052/meta;jsessionid=B3CAB58645372AD4BE86A845 A6464126.ip-10-40-1-105.

[24] P. Bak, C. Tang, and K. Wiesenfeld, "Self-organized criticality: an explanation of the 1/f noise," Physical Review Letters, vol. 59, p. 381, 1987.

[25] M. H. Ansari and L. Smolin, "Self-organized criticality in quantum gravity," Classical and Quantum Gravity, vol. 25, no. 9, 095016, 13 pages, 2008.

[26] J. Ambjorn, J. Gizbert-Studnicki, A. Gorlich, and J. Jurkiewicz, "The effective action in 4-dim CDT. The transfer matrix approach," Journal of High Energy Physics, vol. 34, 2014, https:// link.springer.com/article/10.1007%2FJHEP06%282014%29034.

Jakub Mielczarek

Institute of Physics, Jagiellonian University, Ul. Lojasiewicza 11, 30-348

Krakow, Poland

Correspondence should be addressed to Jakub Mielczarek; jakub.mielczarek@uj.edu.pl

Received 12 May 2017; Accepted 4 July 2017; Published 22 August 2017

Academic Editor: Jerzy Kowalski-Glikman

Caption: FIGURE 1: (a) Ring graph being a toy model of the low temperature geometric state of gravity. (b) Complete graph being a model of high temperature nongeometric state of gravity.

Caption: FIGURE 2: Spectral dimensions for the Ring graph (geometric phase) and the Complete graph (nongeometric phase) with N = 20 nodes.

Caption: FIGURE 3: Modulus of the filed [[phi].sup.[mu]] as a function of the energy density[rho]. The region [rho] > [[rho].sub.c] is forbidden within the model.
COPYRIGHT 2017 Hindawi Limited
No portion of this article can be reproduced without the express written permission from the copyright holder.
Copyright 2017 Gale, Cengage Learning. All rights reserved.

Article Details
Printer friendly Cite/link Email Feedback
Title Annotation:Research Article
Author:Mielczarek, Jakub
Publication:Advances in High Energy Physics
Date:Jan 1, 2017
Words:3443
Previous Article:Localization of Massive and Massless Fermions on Two-Field Branes.
Next Article:SppC Based Energy Frontier Lepton-Proton Colliders: Luminosity and Physics.
Topics:

Terms of use | Privacy policy | Copyright © 2021 Farlex, Inc. | Feedback | For webmasters