DOCSLIB.ORG

Higgs Boson, Renormalization Group, and Cosmology

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
Higgs Boson, Renormalization Group, and Cosmology Hot topics in Modern Cosmology Spontaneous Workshop V, Carg`ese,France Higgs boson, renormalization group, and cosmology A.Yu. Kamenshchik University of Bologna and INFN, Bologna L.D. Landau Institute for Theoretical Physics, Moscow May 9 - May 14, 2011 Based on A.O. Barvinsky, A.Yu. Kamenshchik and A.A. Starobinsky, Inflation scenario via the Standard Model Higgs boson and LHC, JCAP 0811 (2008) 021 A.O. Barvinsky, A.Yu. Kamenshchik, C. Kiefer, A.A. Starobinsky and C. Steinwachs, Asymptotic freedom in inflationary cosmology with a non-minimally coupled Higgs field, JCAP 0912 (2009) 003 Higgs boson, renormalization group, and cosmology, arXiv: 0910.1041 [hep-ph] Content 1. Introduction 2. One-loop approximation 3. Renormalization group 4. Inflationary stage versus post-inflationary running 5. Numerical analysis 6. Conclusions and discussion Introduction The task - the construction of a fundamental particle physics model accounting for an inflationary scenario in cosmology. I A scalar field is very convenient for providing an inflationary stage of the cosmic expansion I A self-interaction of a scalar field creates problems for inflation I The inclusion of the non-minimal coupling ξRφ2 supplies us with an effective potential providing a slow-roll regime for the universe I Due to quantum effects the early evolution of the universe depends not only on the inflaton-graviton sector, but is strongly effected by the particle content of the theory I Main quantum effects are encoded in a special combination of coupling constants A - anomalous scaling I The nature of an inflaton scalar field - could it be the Higgs boson ? I Quantum effects and the renormalization group running I The asymptotical freedom effect for the anomalous scaling I The cosmological model of inflation based on the non-minimally coupled Higgs boson looks as compatible with both : cosmological observations and particle physics bounds, but some details are not yet clear 1 ¡ ¢ 1 λ L(g ,Φ) = M2 + ξ|Φ|2 R − |∇Φ|2 − (|Φ|2 − v 2)2, µν 2 P 2 4 |Φ|2 = Φ†Φ. X 1 X 1 X L = − λ χ2ϕ2 − g 2A2 ϕ2 − y ϕψψ.¯ int 2 χ 2 A µ ψ χ A ψ Quantum one-loop correction to the potential is X m4(ϕ) m2(ϕ) λA ϕ2 (±1) ln = ϕ4 ln + ... 64π2 µ2 128π2 µ2 particles à ! 2 X X X A = λ2 + 3 g 4 − 4 y 4 . λ χ A ψ χ A ψ In the context of quantum cosmology the positivity of the coefficient A makes one-loop wave functions of the universe (both no-boundary and tunneling) normalizable. The anomalous scaling in the case of ξ À 1 determines the quantum rolling force in the effective equation of the inflationary dynamics and yields the parameters of the CMB generated during inflation. For the Standard Model 3 ³ ¡ ¢ ´ A = 2g 4 + g 2 + g 02 2 − 16y 4 . 8λ t In the conventional range of the Higgs mass 115 GeV≤ MH ≤ 180 GeV this quantity at the electroweak scale belongs to the range −48 < A < −20 which strongly contradicts the CMB data which require −12 < A < 14. Taking into account the renormalization group running 3 ³ ¡ ¢ ´ A(t) = 2g 4(t) + g 2(t) + g 02(t) 2 − 16y 4(t) , 8λ(t) t t = ln(ϕ/µ) we see that the value of the A on the inflationary scale is compatible with the CMB data. Our results are in a qualitative agreement with those presented in F.L. Bezrukov, A. Magnin and M. Shaposhnikov, Standard Model Higgs boson mass from inflation, Phys. Lett. B 675, 88 (2009). F. Bezrukov and M. Shaposhnikov, Standard Model Higgs boson mass from inflation: two loop analysis, JHEP 0907, 089 (2009). A. De Simone, M. P. Hertzberg and F. Wilczek, Running Inflation in the Standard Model, Phys. Lett. B 678, 1 (2009). One-loop approximation Z µ ¶ 1 S[g , ϕ] = d 4x g 1/2 −V (ϕ) + U(ϕ) R(g ) − G(ϕ)(∇ϕ)2 µν µν 2 λ λϕ4 ϕ2 V (ϕ) = (ϕ2 − ν2)2 + A ln , 4 128π2 µ2 µ ¶ 1 ϕ2 ϕ2 U(ϕ) = (M2 + ξϕ2) + C ln + D , 2 P 384π2 µ2 µ ¶ 1 ϕ2 G(ϕ) = 1 + F ln + E . 192π2 µ2 From the Jordan frame to the Einstein frame µ ¶2 2 02 2U(ϕ) dϕˆ MP GU + 3U gˆµν = 2 gµν, = 2 . MP dϕ 2 U ˆ 2 ˆ U = MP /2, G = 1, ¯ µ ¶2 ¯ M2 V (ϕ) ¯ Vˆ (ϕ ˆ) = P ¯ . 2 U2(ϕ) ¯ ϕ=ϕ(ϕ ˆ) √ At the inflation scale with ϕ > MP / ξ À v and for large non-minimal coupling ξ À 1 µ ¶ λM4 2M2 A ϕ Vˆ = P 1 − P + I ln , 4 ξ2 ξϕ2 16π2 µ where inflationary anomalous scaling AI is the anomalous scaling modified by the quantum correction to the non-minimal curvature coupling: 3 ¡ ¢ A = A−12λ = 2g 4 + (g 2 + g 02)2 − 16y 4 −6λ. I 8λ t Inflationary slow-roll parameters: à !2 µ ¶ M2 1 dVˆ 4 M2 A 2 εˆ ≡ P = P + I , 2 Vˆ dϕˆ 3 ξ ϕ2 64π2 M2 d 2Vˆ 4M2 ηˆ ≡ P = − P . Vˆ dϕˆ2 3ξϕ2 Their smallness determines the range of the inflationary stage ϕ > ϕend, terminating at the value of εˆ, which we chose to be εˆend = 3/4. Then the inflaton value at the exit from inflation equals √ ϕend ' 2MP / 3ξ. The duration of inflation which starts at ϕ in units of the scale factor e-folding number N: 2 µ ¶ 2 2 ϕ x ln N 2 64π MP 2 = e − 1 + O , ϕI = , ϕI N ξAI NA x ≡ I . 48π2 The CMB spectral index ns , the tensor to scalar ratio r and the spectral index running α: 2 x n = 1 − , s N ex − 1 µ ¶ 12 xex 2 r = , N2 ex − 1 2 x 2ex α = − . N2 (ex − 1)2 Renormalization Group improvement λ(t) V (ϕ) = Z 4(t) ϕ4, 4 1³ ´ U(ϕ) = M2 + ξ(t) Z 2(t) ϕ2 , 2 P G(ϕ) = Z 2(t). dλ dξ dZ = β , = β , = γ. dt λ dt ξ dt These β-functions depend on running couplings λ and ξ as well as on the rest of the coupling constants in Standard Model. 0 dg dg dgs dyt = β , = β 0 , = β , = β . dt g dt g dt gs dt yt The effect of non-minimal curvature coupling of the Higgs field Due to the strong non-minimal coupling between graviton and Higgs-field sectors the propagator of the Higgs field is modified by the factor s(t): U s(ϕ) ≡ GU + 3U02 M2 + ξϕ2 = P . 2 2 2 ˙ 2 MP + ξϕ + 6ϕ (ξ + ξ) At the electroweak scale s(t) ≈ 1, at inflationary scale 1 s(t) ∼ ξ ¿ 1. The one-loop anomalous dimension and β-functions of the Standard Model modified by the s-factor: µ ¶ 1 9g 2 3g 02 γ = + − 3y 2 , 16π2 4 4 t λ ¡ 2 2 ¢ βλ = 2 18s λ + λA(t) − 4γλ, 16π µ ¶ y 2 ³ s ´ β = t − g 02 − 8g 2 + 1 + y 2 − γy , yt 16π2 3 s 2 t t 39 − s g 3 β = − , g 12 16π2 81 + s g 03 β 0 = , g 12 16π2 7g 3 β = − s , gs 16π2 6ξ β = (1 + s2)λ − 2γξ. ξ 16π2 Inflationary stage versus post-inflationary running The inflationary stage in units of a Higgs field e-foldings is very short. We consider the solutions of RG equations at one-loop order and only up to terms linear in ∆t ≡ t − tend = ln(ϕ/ϕend). This approximation will be justified in most of the Higgs mass range compatible with the CMB data. µ ¶ A λ(t) = λ 1 − 4γ ∆t + end ∆t , end end 16π2 ³ ´ ξ(t) = ξend 1 − 2γend∆t . Here λend, γend, ξend are determined at tend and Aend = A(tend) is a value of the running anomalous scaling at the end of inflation. The renormalization group improved potential µ ¶ M2 2 V λ(t) Vˆ = P ' M4 2 U2 P 4ξ2(t) µ 2 ¶ 4 λend 2MP AI(tend) φ = MP 2 1 − 2 + 2 ln . 4ξend ξendφ 16π φend Our ”old” formalism can be directly applied to determine the parameters of the CMB. They are mainly determined by the anomalous scaling AI, this quantity should be taken at tend. We integrate the renormalization group equations from the top quark mass scale µ = Mt = 171Gev. The initial condition ξ(0) is not known. It should be determined from the CMB normalization condition for the amplitude of the power spectrum, which yields µ ¶2 λin −9 xin exp xin 2 ' 0.5 × 10 ξin exp xin − 1 at the moment of the first horizon crossing for N = 60 which we call the “beginning” of inflation tin. This moment can be determined from the relation MP 1 4N 1 exp xin − 1 tin = ln + ln + ln . Mt 2 3ξin 2 xin The end of inflation: MP 1 4 tend = ln + ln . Mt 2 3ξend The duration of inflation in units of inflaton field e-foldings tin − tend = ln(ϕin/ϕend) is very short relative to the post-inflationary evolution tend ∼ 35, 1 1 ξin 1 exp xin − 1 1 tin − tend = ln N + ln + ln ' ln N ∼ 2. 2 2 ξend 2 xin 2 The coefficient A which has a big negative values at the electroweak scale becomes rather small at the inflationary scale - asymptotic freedom. Numerical analysis The running of A(t) depends on the behavior of λ(t). For small Higgs masses the usual RG flow leads to an instability of the electroweak vacuum caused by negative values of λ(t) in a certain range of t.
Load more

Recommended publications
  • Path Integral Formulation of Loop Quantum Cosmology
    Path Integral Formulation of Loop Quantum Cosmology Adam D. Henderson Institute for Gravitation and the Cosmos Pennsylvania State University International Loop Quantum Gravity Seminar March 17 2008 Motivations 1. There have been arguments against the singularity resolution in LQC using path integrals. The canonical quantization is well understood and the singularity resolution is robust, so where do the path integral arguments break down? 2. Recent developements have allowed for the construction of new spin foam models that are more closely related to the canonical theory. It is important to make connections to spin-foams by building path integrals from the canonical theory when possible. 3. A path integral representation of Loop Quantum Cosmology will aid in studying the physics of more complicated LQC models (k = 1, Λ = 0, Bianchi). Using standard path integral techniques one can 6 argue why the effective equations are so surprisingly accurate. Introduction We construct a path integral for the exactly soluble Loop Quantum • Cosmology starting with the canonical quantum theory. The construction defines each component of the path integral. Each • has non-trivial changes from the standard path integral. We see the origin of singularity resolution in the path integral • representation of LQC. The structure of the path integral features similarities to spin foam • models. The path integral can give an argument for the surprising accuracy • of the effective equations used in more complicated models. Outline Standard Construction Exactly Soluble LQC LQC Path Integral Other Forms of Path Integral Singularity Resolution/Effective Equations Conclusion Path Integrals - Overview Path Integrals: Covariant formulation of quantum theory expressed • as a sum over paths Formally the path integral can be written as • qeiS[q]/~ or q peiS[q,p]/~ (1) D D D Z Z To define a path integral directly involves defining the components • of these formal expressions: 1.
    [Show full text]
  • Prediction in Quantum Cosmology
    Prediction in Quantum Cosmology James B. Hartle Department of Physics University of California Santa Barbara, CA 93106, USA Lectures at the 1986 Carg`esesummer school publshed in Gravitation in As- trophysics ed. by J.B. Hartle and B. Carter, Plenum Press, New York (1987). In this version some references that were `to be published' in the original have been supplied, a few typos corrected, but the text is otherwise unchanged. The author's views on the quantum mechanics of cosmology have changed in important ways from those originally presented in Section 2. See, e.g. [107] J.B. Hartle, Spacetime Quantum Mechanics and the Quantum Mechan- ics of Spacetime in Gravitation and Quantizations, Proceedings of the 1992 Les Houches Summer School, ed. by B. Julia and J. Zinn-Justin, Les Houches Summer School Proceedings Vol. LVII, North Holland, Amsterdam (1995).) The general discussion and material in Sections 3 and 4 on the classical geom- etry limit and the approximation of quantum field theory in curved spacetime may still be of use. 1 Introduction As far as we know them, the fundamental laws of physics are quantum mechanical in nature. If these laws apply to the universe as a whole, then there must be a description of the universe in quantum mechancial terms. Even our present cosmological observations require such a description in principle, although in practice these observations are so limited and crude that the approximation of classical physics is entirely adequate. In the early universe, however, the classical approximation is unlikely to be valid. There, towards the big bang singularity, at curvatures characterized by the Planck length, 3 1 (¯hG=c ) 2 , quantum fluctuations become important and eventually dominant.
    [Show full text]
  • Vacuum Energy
    Vacuum Energy Mark D. Roberts, 117 Queen’s Road, Wimbledon, London SW19 8NS, Email:[email protected] http://cosmology.mth.uct.ac.za/ roberts ∼ February 1, 2008 Eprint: hep-th/0012062 Comments: A comprehensive review of Vacuum Energy, which is an extended version of a poster presented at L¨uderitz (2000). This is not a review of the cosmolog- ical constant per se, but rather vacuum energy in general, my approach to the cosmological constant is not standard. Lots of very small changes and several additions for the second and third versions: constructive feedback still welcome, but the next version will be sometime in coming due to my sporadiac internet access. First Version 153 pages, 368 references. Second Version 161 pages, 399 references. arXiv:hep-th/0012062v3 22 Jul 2001 Third Version 167 pages, 412 references. The 1999 PACS Physics and Astronomy Classification Scheme: http://publish.aps.org/eprint/gateway/pacslist 11.10.+x, 04.62.+v, 98.80.-k, 03.70.+k; The 2000 Mathematical Classification Scheme: http://www.ams.org/msc 81T20, 83E99, 81Q99, 83F05. 3 KEYPHRASES: Vacuum Energy, Inertial Mass, Principle of Equivalence. 1 Abstract There appears to be three, perhaps related, ways of approaching the nature of vacuum energy. The first is to say that it is just the lowest energy state of a given, usually quantum, system. The second is to equate vacuum energy with the Casimir energy. The third is to note that an energy difference from a complete vacuum might have some long range effect, typically this energy difference is interpreted as the cosmological constant.
    [Show full text]
  • Spontaneous Symmetry Breaking and Mass Generation As Built-In Phenomena in Logarithmic Nonlinear Quantum Theory
    Vol. 42 (2011) ACTA PHYSICA POLONICA B No 2 SPONTANEOUS SYMMETRY BREAKING AND MASS GENERATION AS BUILT-IN PHENOMENA IN LOGARITHMIC NONLINEAR QUANTUM THEORY Konstantin G. Zloshchastiev Department of Physics and Center for Theoretical Physics University of the Witwatersrand Johannesburg, 2050, South Africa (Received September 29, 2010; revised version received November 3, 2010; final version received December 7, 2010) Our primary task is to demonstrate that the logarithmic nonlinearity in the quantum wave equation can cause the spontaneous symmetry break- ing and mass generation phenomena on its own, at least in principle. To achieve this goal, we view the physical vacuum as a kind of the funda- mental Bose–Einstein condensate embedded into the fictitious Euclidean space. The relation of such description to that of the physical (relativis- tic) observer is established via the fluid/gravity correspondence map, the related issues, such as the induced gravity and scalar field, relativistic pos- tulates, Mach’s principle and cosmology, are discussed. For estimate the values of the generated masses of the otherwise massless particles such as the photon, we propose few simple models which take into account small vacuum fluctuations. It turns out that the photon’s mass can be naturally expressed in terms of the elementary electrical charge and the extensive length parameter of the nonlinearity. Finally, we outline the topological properties of the logarithmic theory and corresponding solitonic solutions. DOI:10.5506/APhysPolB.42.261 PACS numbers: 11.15.Ex, 11.30.Qc, 04.60.Bc, 03.65.Pm 1. Introduction Current observational data in astrophysics are probing a regime of de- partures from classical relativity with sensitivities that are relevant for the study of the quantum-gravity problem [1,2].
    [Show full text]
  • Spin Foam Vertex Amplitudes on Quantum Computer—Preliminary Results
    universe Article Spin Foam Vertex Amplitudes on Quantum Computer—Preliminary Results Jakub Mielczarek 1,2 1 CPT, Aix-Marseille Université, Université de Toulon, CNRS, F-13288 Marseille, France; [email protected] 2 Institute of Physics, Jagiellonian University, Łojasiewicza 11, 30-348 Cracow, Poland Received: 16 April 2019; Accepted: 24 July 2019; Published: 26 July 2019 Abstract: Vertex amplitudes are elementary contributions to the transition amplitudes in the spin foam models of quantum gravity. The purpose of this article is to make the first step towards computing vertex amplitudes with the use of quantum algorithms. In our studies we are focused on a vertex amplitude of 3+1 D gravity, associated with a pentagram spin network. Furthermore, all spin labels of the spin network are assumed to be equal j = 1/2, which is crucial for the introduction of the intertwiner qubits. A procedure of determining modulus squares of vertex amplitudes on universal quantum computers is proposed. Utility of the approach is tested with the use of: IBM’s ibmqx4 5-qubit quantum computer, simulator of quantum computer provided by the same company and QX quantum computer simulator. Finally, values of the vertex probability are determined employing both the QX and the IBM simulators with 20-qubit quantum register and compared with analytical predictions. Keywords: Spin networks; vertex amplitudes; quantum computing 1. Introduction The basic objective of theories of quantum gravity is to calculate transition amplitudes between configurations of the gravitational field. The most straightforward approach to the problem is provided by the Feynman’s path integral Z i (SG+Sf) hY f jYii = D[g]D[f]e } , (1) where SG and Sf are the gravitational and matter actions respectively.
    [Show full text]
  • On the Fate of Singularities in Quantum Gravity
    On the fate of singularities in quantum gravity Claus Kiefer Institut f¨ur Theoretische Physik Universitat¨ zu Koln¨ ½ Contents Singularities in cosmology Quantum geometrodynamics Quantum cosmology Quantum gravitational collapse Singularities in the classical theory Definition of a singularity A spacetime is singular if it is incomplete with respect to a timelike or null geodesic and if it cannot be embedded in a bigger spacetime. ◮ Energy condition ◮ Condition on the global structure ◮ Gravitation strong enough to lead to the existence of a closed trapped surface Theorem (Hawking and Penrose 1970) A spacetime M cannot satisfy causal geodesic completeness if, together with Einstein’s equations, the following four conditions hold: 1. M contains no closed timelike curves. 2. The strong energy condition is satisfied at every point. 3. The generality condition (. ) is satisfied for every causal geodesic. 4. M contains either a trapped surface, or a point p for which the convergence of all the null geodesics through p changes sign somewhere to the past of p, or a compact spacelike hypersurface Strong energy condition: ρ + p 0, ρ + p 0, i = 1, 2, 3 i i ≥ i ≥ P Cosmological singularities for homogeneous and isotropic spacetimes Classified by behaviour of scale factor a, energy density ρ, pressure p: Big Bang/Crunch a = 0 at finite proper time, ρ diverges Type I (Big Rip) a diverges in finite proper time, ρ and p diverge Type II or “sudden” (Big Brake/Big Demarrage)´ a finite, ρ finite, p diverges, Hubble parameter finite Type III (Big Freeze) a finite, both ρ and p diverge Type IV a finite, both ρ and p finite, but curvature derivatives diverge Most of these singularities occur in spite of the violation of energy conditions Relation to observations The observation of the Cosmic Microwave Background Radiation (CMB) indicates that there is enough matter on the past light-cone of our present location P to imply that the divergence of this cone changes somewhere to the past of P .
    [Show full text]
  • Propagator for the Free Relativistic Particle on Archimedean and Nonarchimedean Spaces Udc: 530.1
    FACTA UNIVERSITATIS Series: Physics, Chemistry and Technology Vol. 3, No 1, 2004, pp. 9-21 PROPAGATOR FOR THE FREE RELATIVISTIC PARTICLE ON ARCHIMEDEAN AND NONARCHIMEDEAN SPACES UDC: 530.1 D. D. Dimitrijević, G. S. Djordjević and Lj. Nešić Faculty of Science and Mathematics, P.O. Box 224, 18001 Niš, Serbia and Montenegro Abstract. We consider dynamics of a free relativistic particle at very short distances, treating space-time as archimedean as well as nonarchimedean one. Usual action for the relativistic particle is nonlinear. Meanwhile, in the real case, that system may be treated like a system with quadratic (Hamiltonian) constraint. We perform similar procedure in p -adic case, as the simplest example of a nonarchimedean space. The existence of the simplest vacuum state is considered and corresponding Green function is calculated. Similarities and differences between obtained results on both spaces are examined and possible physical implications are discussed. 1. INTRODUCTION It is generally believed that the notion of space-time as a continuous manifold should −35 break down at very short distances of the order of the Planck length λp ~ 10 m . This would arise from the process of measurement of space-time points based on quantum mechanics and gravity arguments [1]. Among many different possibilities for a mathematical background of a quantum theory on very small distances, noncommutative [2] and nonarchimedan [3] spaces appear as the most promising ones. The simplest example of a nonarchimedean space, and the most suitable mathematical machinery for describing it, comes from the theory of p-adic numbers and p-adic analysis. Since 1987, there has been an important interest in application of p -adic numbers in many branches of theoretical and mathematical physics (for a review, see [4]).
    [Show full text]
  • The Quantum Vacuum and the Cosmological Constant Problem
    The Quantum Vacuum and the Cosmological Constant Problem S.E. Rugh∗and H. Zinkernagel† Abstract - The cosmological constant problem arises at the intersection be- tween general relativity and quantum field theory, and is regarded as a fun- damental problem in modern physics. In this paper we describe the historical and conceptual origin of the cosmological constant problem which is intimately connected to the vacuum concept in quantum field theory. We critically dis- cuss how the problem rests on the notion of physical real vacuum energy, and which relations between general relativity and quantum field theory are assumed in order to make the problem well-defined. Introduction Is empty space really empty? In the quantum field theories (QFT’s) which underlie modern particle physics, the notion of empty space has been replaced with that of a vacuum state, defined to be the ground (lowest energy density) state of a collection of quantum fields. A peculiar and truly quantum mechanical feature of the quantum fields is that they exhibit zero-point fluctuations everywhere in space, even in regions which are otherwise ‘empty’ (i.e. devoid of matter and radiation). These zero-point arXiv:hep-th/0012253v1 28 Dec 2000 fluctuations of the quantum fields, as well as other ‘vacuum phenomena’ of quantum field theory, give rise to an enormous vacuum energy density ρvac. As we shall see, this vacuum energy density is believed to act as a contribution to the cosmological constant Λ appearing in Einstein’s field equations from 1917, 1 8πG R g R Λg = T (1) µν − 2 µν − µν c4 µν where Rµν and R refer to the curvature of spacetime, gµν is the metric, Tµν the energy-momentum tensor, G the gravitational constant, and c the speed of light.
    [Show full text]
  • Making a Quantum Universe: Symmetry and Gravity
    Article Making a Quantum Universe: Symmetry and Gravity Houri Ziaeepour1,2 1 Institut UTINAM, CNRS UMR 6213, Observatoire de Besançon, Université de Franche Compté, 41 bis ave. de l’Observatoire, BP 1615, 25010 Besançon, France; 2 Mullard Space Science Laboratory, University College London, Holmbury St. Mary, GU5 6NT, Dorking, UK; [email protected] Version October 14, 2020 submitted to Universe Abstract: So far none of attempts to quantize gravity has led to a satisfactory model that not only describe gravity in the realm of a quantum world, but also its relation to elementary particles and other fundamental forces. Here we outline preliminary results for a model of quantum universe, in which gravity is fundamentally and by construction quantic. The model is based on 3 well motivated assumptions with compelling observational and theoretical evidence: quantum mechanics is valid at all scales; quantum systems are described by their symmetries; Universe has infinite independent degrees of freedom. The last assumption means that the Hilbert space of the Universe has SUpN Ñ 8q – area preserving Diff.pS2q symmetry, which is parameterized by two angular variables. We show that in absence of a background spacetime, this Universe is trivial and static. Nonetheless, quantum fluctuations break the symmetry and divide the Universe to subsystems. When a subsystem is singled out as reference - observer - and another as clock, two more continuous parameters arise, which can be interpreted as distance and time. We identify the classical spacetime with parameter space of the Hilbert space of the Universe. Therefore, its quantization is meaningless. In this view, the Einstein equation presents the projection of quantum dynamics in the Hilbert space into its parameter space.
    [Show full text]
  • Quantum Propagation Across Cosmological Singularities
    Quantum propagation across cosmological singularities Steffen Gielen Theoretical Physics, Blackett Laboratory, Imperial College London, London SW7 2AZ, United Kingdom Perimeter Institute for Theoretical Physics, Waterloo, Ontario N2L 2Y5, Canada and Canadian Institute for Theoretical Astrophysics (CITA), 60 St George Street, Toronto, Ontario M5S 3H8, Canada Neil Turok Perimeter Institute for Theoretical Physics, Waterloo, Ontario N2L 2Y5, Canada (Dated: May 14, 2017) The initial singularity is the most troubling feature of the standard cosmology, which quantum effects are hoped to resolve. In this paper, we study quantum cosmology with conformal (Weyl invariant) matter. We show that it is natural to extend the scale factor to negative values, allowing a large, collapsing universe to evolve across a quantum \bounce" into an expanding universe like ours. We compute the Feynman propagator for Friedmann-Robertson-Walker backgrounds exactly, identifying curious pathologies in the case of curved (open or closed) universes. We then include anisotropies, fixing the operator ordering of the quantum Hamiltonian by imposing covariance under field redefinitions and again finding exact solutions. We show how complex classical solutions allow one to circumvent the singularity while maintaining the validity of the semiclassical approximation. The simplest isotropic universes sit on a critical boundary, beyond which there is qualitatively different behavior, with potential for instability. Additional scalars improve the theory's stability. Finally, we study the semiclassical propagation of inhomogeneous perturbations about the flat, isotropic case, at linear and nonlinear order, showing that, at least at this level, there is no particle production across the bounce. These results form the basis for a promising new approach to quantum cosmology and the resolution of the big bang singularity.
    [Show full text]
  • Quintessential Inflation with Dynamical Higgs
    S S symmetry Article Quintessential Inflation with Dynamical Higgs Generation as an Affine Gravity David Benisty 1,2, Eduardo I. Guendelman 1,2,3, Emil Nissimov 4,* and Svetlana Pacheva 4 1 Physics Department, Ben-Gurion University of the Negev, Beer-Sheva 84105, Israel; [email protected] (D.B.); guendelman@fias.uni-frankfurt.de (E.I.G.) 2 Frankfurt Institute for Advanced Studies (FIAS), Ruth-Moufang-Strasse 1, 60438 Frankfurt am Main, Germany 3 Bahamas Advanced Study Institute and Conferences, 4A Ocean Heights, Hill View Circle, Stella Maris, Long Island, Bahamas 4 Institute for Nuclear Research and Nuclear Energy, Bulgarian Academy of Sciences, 1784 Sofia, Bulgaria; [email protected] * Correspondence: [email protected] Received: 16 March 2020; Accepted: 13 April 2020; Published: 5 May 2020 Abstract: First, we propose a scale-invariant modified gravity interacting with a neutral scalar inflaton and a Higgs-like SU(2) × U(1) iso-doublet scalar field based on the formalism of non-Riemannian (metric-independent) spacetime volume-elements. This model describes, in the physical Einstein frame, a quintessential inflationary scenario driven by the “inflaton” together with the gravity-“inflaton” assisted dynamical spontaneous SU(2) × U(1) symmetry breaking in the post-inflationary universe, whereas the SU(2) × U(1) symmetry remains intact in the inflationary epoch. Next, we find the explicit representation of the latter quintessential inflationary model with a dynamical Higgs effect as an Eddington-type purely affine gravity. Keywords: inflation; dark energy; dynamical Higgs effect; quintessence 1. Introduction Studies in cosmology are dominated by the fundamental concept of “inflation”—a period of exponential expansion, which provides a plausible solution for the “puzzles” of the Big-Bang cosmology (the horizon problem, the flatness problem, the magnetic monopole problem, etc.) [1–8].
    [Show full text]
  • The Quantum Vacuum and the Cosmological Constant Problem
    The Quantum Vacuum and the Cosmological Constant Problem S.E. Rugh∗and H. Zinkernagely To appear in Studies in History and Philosophy of Modern Physics Abstract - The cosmological constant problem arises at the intersection be- tween general relativity and quantum field theory, and is regarded as a fun- damental problem in modern physics. In this paper we describe the historical and conceptual origin of the cosmological constant problem which is intimately connected to the vacuum concept in quantum field theory. We critically dis- cuss how the problem rests on the notion of physically real vacuum energy, and which relations between general relativity and quantum field theory are assumed in order to make the problem well-defined. 1. Introduction Is empty space really empty? In the quantum field theories (QFT’s) which underlie modern particle physics, the notion of empty space has been replaced with that of a vacuum state, defined to be the ground (lowest energy density) state of a collection of quantum fields. A peculiar and truly quantum mechanical feature of the quantum fields is that they exhibit zero-point fluctuations everywhere in space, even in regions which are otherwise ‘empty’ (i.e. devoid of matter and radiation). These zero-point fluctuations of the quantum fields, as well as other ‘vacuum phenomena’ of quantum field theory, give rise to an enormous vacuum energy density ρvac. As we shall see, this vacuum energy density is believed to act as a contribution to the cosmological constant Λ appearing in Einstein’s field equations from 1917, 1 8πG R g R Λg = T (1) µν − 2 µν − µν c4 µν where Rµν and R refer to the curvature of spacetime, gµν is the metric, Tµν the energy-momentum tensor, G the gravitational constant, and c the speed of light.
    [Show full text]