DOCSLIB.ORG

Implications of the Curvaton on Inflationary Cosmology

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
Implications of the Curvaton on Inflationary Cosmology Implications of the Curvaton on Inflationary Cosmology March 4, 2005 @ KEK, Tsukuba KEK theory meeting 2005 “Particle Physics Phenomenology” Tomo Takahashi ICRR, University of Tokyo Collaborators: Takeo Moroi (Tohoku) Yoshikazu Toyoda (Tohoku) 1. Introduction Inflation (a superluminal expansion at the early universe) [Guth 1980, Sato 1980] is one of the most promising ideas to solve the horizon and flatness problem. The potential energy of a scalar field (inflaton) causes inflation. ★ Inflation can also provide the seed of cosmic density perturbations today. Quantum fluctuation of the inflaton field during inflation can be the origin of today’s cosmic fluctuation. From observations of CMB, large scale structure, we can obtain constraints on inflation models. However, fluctuation can be provided by some sources other than fluctuation of the inflaton. From the viewpoint of particle physics, there can exist scalar fields other than the inflaton. (late-decaying moduli, Affleck-Dine fields, right-handed sneutrino...) What if another scalar field acquires primordial fluctuation? Such a field can also be the origin of today’s fluctuation. Curvaton field (since it can generate the curvature perturbation.) [Enqvist & Sloth, Lyth & Wands, Moroi & TT 2001] ★Generally, fluctuation of inflaton and curvaton can be both responsible for the today’s density fluctuation. What is the implication of the curvaton for This talk ➡ constraints on models of inflation? 2. Generation of fluctuations: Standard case Primordial fluctuation: the standard case a˙ H H ≡ :Hubble parameter The quantum fluctuation of the inflaton δχ ∼ a 2π dχ χ˙ ≡ H dt The curvature perturbation R ∼ − δχ χ˙ The power spectrum of R . Inflation RD MD (The initial power spectrum) Scale horizon scale 2 2 2 H H horizon crossing PR(k) ∼< R >∼ ! χ˙ " !2π " #k=aH # # Inside the horizon Almost scale-invariant spectrum Scale factor a reheating ns−1 Generally, it can be written as a power-law form; PR ∝ k ★ ns depends on models of inflation What is the discriminators of models of inflation? ns−1 The initial power spectrum ( P R ∝ k ) depends on models. During inflation, the gravity waves are also produced. The size of gravity waves (tensor mode) also depends on models. The observable quantities d ln P n n − 1 ≡ R Scalar spectral index s s d ln k ! "k=aH # P " Tensor-scalar ratio r ≡ grav " PR ( Overall normalization of PR ) These parameters can be determined from observations. (such as CMB, large scale structure and so on.) Constraints on models of inflation. Constraints from current observations [Leach, Liddle 2003 ] [Data from CMB (WMAP, VSA, ACBAR) and large scale structure (2dF) are used.] 0.5 ★ Some inflation models are 6 V ∼ χ already excluded! 0.4 V ∼ χ4 Example: chaotic inflation 0.3 α r r 4 χ ∼ 2 V (χ) = λMpl V χ M 0.2 ! pl " 99% 95% ★ The cases with α = 4, 6, · · · are almost excluded. 0.1 0 !0.08 !0.04 0 0.04 nn −!11 s s The observable quantities can be written with the slow-roll parameters. 1 V ! 2 1 V !! where ! ≡ η ≡ ! dV (χ) Slow-roll parameters, 2M 2 V 2 V (χ) ≡ pl ! " Mpl V dχ dV (χ) dχ χ¨ + 3Hχ˙ + = 0 where χ˙ ≡ Equation of motion for a scalar field: dχ dt dV (χ) When it slowly rolls down the potential, 3Hχ˙ + ! 0 dχ (Slow-roll approximation) ★ The slow-roll approximation is valid when ! , | η | ! 1 . The scalar spectral index ns − 1 = 4η − 6" P The tensor-scalar ratio r = grav = 16! PR 3. Curvaton mechanism [Enqvist & Sloth, Lyth & Wands, Moroi & TT 2001] Curvaton: a light scalar field which is partially or totally responsible for the density fluctuation. (Usually, quantum fluctuation of the inflaton is assumed to be totally responsible for that.) Roles of the inflaton and the curvaton Inflaton ➡ causes the inflation, not fully responsible for the cosmic fluctuation Curvaton ➡ is not responsible for the inflation, is fully or partially responsible for the cosmic fluctuation Constraints on inflation models can be relaxed. Thermal history of the universe with the curvaton Curvaton Inflation RD Inflation RD1 RD2 dominated (Standard case) inflaton y density y density curvaton Energ !BBN Energ reheating Time !BBN reheating reheating Time (For simplicity, an oscillating inflaton period is omitted.) 1 = 2 2 The potential of the curvaton is assumed as Vcurvaton 2mφφ The oscillating field behaves as matter. Thermal history of the universe with the curvaton H > mφ V (φ) Inflation Curvaton RD1 dominated RD2 inflaton y density curvaton φ Energ V (φ) H ∼ mφ !BBN reheating reheating Time φ (For simplicity, an oscillating inflaton period is omitted.) 1 = 2 2 The potential of the curvaton is assumed as Vcurvaton 2mφφ The oscillating field behaves as matter. Density Perturbation Fluctuation of the inflaton Curvature perturbation H δχ ∼ H ! 2π " R ∼ − δχ χ˙ Fluctuation of the curvaton No curvature perturbation H δφ ∼ (The curvaton is subdominant component during inflation.) ! 2π " However, isocurvature fluctuation can be generated. 2δφinit Sφχ ∼ δχ − δφ = φinit Curvaton becomes dominant δρi Inflaton where δi ≡ ρi At some point, the curvaton curvaton dominates the universe. the isocurvature fluc.becomes adiabatic (curvature) fluc. After the decay of the curvaton, the curvature fluctuation becomes [Langlois, Vernizzi, 2004] R 1 Vinf 3 δφinit RD2 = 2 ! δχinit + f(X) Mpl Vinf 2 Mpl where X = φinit/Mpl From inflaton From curvaton f(X): represents the size of contribution from the curvaton 9 2 Vinf PR f˜ X ! The power spectrum (scalar mode) = !1 + ( ) " 2 4 4 54π Mpl! where f˜ = (3/√2)f 2 H 2 P = The tensor mode spectrum is not modified. grav M 2 2π pl ! " The scalar spectral index and tensor-scalar ratio with the curvaton 2 − 4 16! η ! r = ns − 1 = −2! + , ˜2 1 + f˜2! 1 + f ! (Notice: the standard case n s − 1 = 4 η − 6 " , r = 16 ! ) Contribution from the curvaton R 1 Vinf 3 δφinit RD2 = 2 ! δχinit + f(X) Mpl Vinf 2 Mpl f(X) can be obtained solving a linear perturbation theory. For small and large limit, [Langlois, Vernizzi, 2004] 4 4 : φinit " Mpl 9X ! 3.5 f(X) 1 X : φ # M 3 init pl 3 ) 2.5 ) X * ( ! 2 ( f f 1.5 1 ★ Small and large initial amplitude 0.5 give large curvaton contributions. 0 0 1 2 3 4 5 6 7 8 9 10 ! /M X(= φ*initpl/Mpl) Relaxing constraint on inflation models with curvaton [Langlois & Vernissi 2004; Moroi, TT & Toyoda 2005] 4 An example: the chaotic inflation with the quartic potential Vinf = λχ 0.5 Without the curvaton (i.e., the standard case) 0.4 ns − 1 ∼ −0.05, r ∼ 0.27 4 V ∼ χ (Assuming N=60) 0.3 r r With the curvaton, 0.2 for φinit = 0.1Mpl 99% 95% 0.1 ns − 1 ∼ −0.04, r ∼ 0.08 ★ 0 !0.08 !0.04 0 0.04 nn −!11 s s The model becomes viable due to the curvaton! Model parameter dependence [Moroi, TT & Toyoda 2005] ★ Whether inflation models can be relaxed or not depends on the model parameters in the curvaton sector. Model parameters in the curvaton sector Initial amplitude of φ : φinit affects the amplitude of fluctuation and the background evolution Mass of φ : mφ affects the background evolution Decay rate of φ : Γφ RDI RD2 Inflation φD MD (standard case) Scale horizon scale Inflation RD MD horizon crossing Inside the horizon reheating Scale factor a Model parameter dependence: Case with the chaotic inflation 4 ★ Potential: Vinf = λχ The region where the curvaton causes the second inflation. [Moroi, TT & Toyoda 2005] 101 The criterion for the alleviation of the model ) pl 0 10 −18 /M Γφ = 10 GeV init F = X( 10-1 −10 w/o curvaton Γφ = 10 GeV 99 % C.L. r 10-2 2 3 4 5 6 7 8 9 10 10 10 10 10 10 10 10 10 10 ★ Not allowed ★ mF (GeV) Allowed 99% ns − 1 ★ The case with large initial amplitude cannot liberate the model, although contribution from the curvaton fluc. is large. Case with the natural inflation [Freese, Friemann, Olint, Adams,Bond, Freese, Frieman,Olint,1990] 4 χ Potential: Vinf = Λ 1 − cos The scalar spectral index ! "F #$ 1 0.95 ) 0.9 E COB (k s n 0.85 0.8 101 0.75 4 5 7 10 20 18 F (10 GeV) [Moroi, TT 2000] ) 0 pl 10 /M 2 init 1 Mpl 1 F ! = 2 = 10-1 2 ! F " tan (χ/2F ) X( 2 95 % C.L. 1 Mpl 1 -2 − 10 η = 2 1 5 6 7 8 9 10 2 ! F " #tan (χ/2F ) $ F (1018 GeV) [Moroi, TT & Toyoda 2005] Case with the new inflation [Linde; Albrecht, Steinhardt 1982] n 2n 2 4 χ χ Potential: Vinf = λ v 1 2 + [Kumekawa, Moroi, Yanagida 1994; − √2v √2v Izawa, Yanagida1997] ! " # " # $ 101 The scalar spectral index n − 1 1 n − 1 = −2 ) 0 s pl 10 n − 2 Ne /M init The tensor-scalar ratio F 2(n−1) = -1 M 2 v 2 n−2 10 1 1 X( ! = n2 pl v n(n − 2) M Ne ! " # ! pl " $ -2 99 % C.L. 1 v 6 10 n = 3 ! = 18 19 for , 4 10 10 9Ne !Mpl " v(GeV) r is small for v ! Mpl [Moroi, TT & Toyoda 2005] Case with Curvaton Curvaton cannot liberate the model, 2η − 4! ns − 1 = −2! + when ! is very small. 1 + f˜2! 5. Summary ★ Current cosmological observation such as CMB, LSS give severe constraints on inflation models. ★ However, if we introduce the curvaton, primordial fluctuation can be also provided by the curvaton field. ★ As a consequence, constraints on inflation models cannot be applied in such a case.
Load more

Recommended publications
  • Higgs As Curvaton in Asymptotic Safe Gravity Scenario
    Higgs As Curvaton in Asymptotic Safe Gravity Scenario Taotao Qiu LeCosPA Center, National Taiwan University 2013/06/17 Based on: Y.-F. Cai, Y.-C. Chang, P. Chen, D. A. Easson1 , T. Qiu, arXiv:1304.6938 [hep-th]. Outline Higgs vs. Cosmology Preliminary of Asyptotic Safe Gravity Our model of Higgs Curvaton in ASG background perturbation non-Gaussianities contraints form Planck data Conclusion 2 Higgs vs. Cosmology 3 The discovery of Higgs Boson Recently, two groups (ATLAS and CMS) in LHC experiment have confirmed the existence of Higgs boson particles predicted in standard model particle physics with the mass value CMS Collaboration 4 ATLAS Collaboration Can Higgs play a role in Cosmology? Connecting cosmology with particle physics: Scalar fields: cosmology Particle physics inflaton, curvaton, Higgs boson quintessence…… Attempts & Problems: Higgs inflation unitarity problem C. P. Burgess, H. M. Lee and M. Trott, JHEP 0909, 103 (2009). Higgs curvaton Too small energy density ratio cannot give rise to enouph perturbation. T. Kunimitsu and J. 'i. Yokoyama, Phys. Rev. D 86, 083541 (2012); K. -Y. Choi and Q. -G. Huang, arXiv:1209.22775 [hep-ph]. The problem of Higgs as a curvaton The problem of Higgs curvaton: When Higgs is to be curvaton, the value of Higgs field h remains constant till the curvaton decays, when the effective mass is close to Hubble parameter: which induces Too small to fit the observational data! K. -Y. Choi and Q. -G. Huang, arXiv:1209.2277 [hep-ph]. Can the problem be solved in framework of Asymptotic Safe Gravity? 6 Preliminary of Asyptotic Safe Gravity 7 Problem: Quantization of Gravity In quantum field theory, people often check the renormaliza- bility of any terms in Lagrangian by its coupling constant! Consider the operator in the lagrangian: renormalizable Super- renormalizable non- renormalizable Another non-renormalizable example is the operator of Einstein- Hilbert Gravity , whose coupling constant is with 8 What is Asymptotic Safe Gravity (ASG) Proposal 1970’s by Steven Weinberg S.
    [Show full text]
  • Higgs Boson in RG Running Inflationary Cosmology
    Higgs Boson in RG running Inflationary Cosmology 1,2, 1, Yi-Fu Cai ∗ and Damien A. Easson † 1Department of Physics, Arizona State University, Tempe, AZ 85287 2Department of Physics, McGill University, Montr´eal, QC, H3A 2T8, Canada An intriguing hypothesis is that gravity may be non-perturbatively renormalizable via the notion of asymptotic safety. We show that the Higgs sector of the SM minimally coupled to asymptotically safe gravity can generate the observed near scale-invariant spectrum of the Cosmic Microwave Back- ground through the curvaton mechanism. The resulting primordial power spectrum places an upper bound on the Higgs mass, which for finely tuned values of the curvaton parameters, is compatible with the recently released Large Hadron Collider data. PACS numbers: 98.80.Cq I. INTRODUCTION play an important role in the early inflationary universe if the gravitational theory is asymptotically safe. Although at present there is no explicit proof of the asymptotical Weinberg has suggested that the effective description safety, it deserves to ask whether the gravity theories un- of a quantum gravitational theory may be nonperturba- der asymptotical safety are testable in any experiment. tively renormalizable through the notion of asymptotic The current study is exactly based on a specific trunca- safety (AS) [1, 2]. In such a scenario the renormalization tion of the gravity action and certain form of RG equa- group (RG) flows approach a fixed point in the ultravio- tions according to the conjecture of asymptotical safety. let (UV) limit, and a finite dimensional critical surface of In the frame of AS gravity, the gravitational constant trajectories evolves to this point at short distance scales G and cosmological constant Λ are running along with [3, 4].
    [Show full text]
  • Implications of Gravitational Waves for Supersymmetric Grand Unification
    PHYSICAL REVIEW D 104, 035031 (2021) Implications of gravitational waves for supersymmetric grand unification So Chigusa ,1,2,3 Yuichiro Nakai,4 and Jiaming Zheng4 1Berkeley Center for Theoretical Physics, Department of Physics, University of California, Berkeley, California 94720, USA 2Theoretical Physics Group, Lawrence Berkeley National Laboratory, Berkeley, California 94720, USA 3KEK Theory Center, IPNS, KEK, Tsukuba, Ibaraki 305-0801, Japan 4Tsung-Dao Lee Institute and School of Physics and Astronomy, Shanghai Jiao Tong University, 800 Dongchuan Road, Shanghai, 200240 China (Received 22 November 2020; accepted 26 July 2021; published 27 August 2021) Supersymmetric grand unification based on SOð10Þ is one of the most attractive paradigms in physics beyond the Standard Model. Inspired by the recent NANOGrav signal, we discuss the implications of detecting a stochastic gravitational wave background emitted by a network of cosmic strings for the SOð10Þ grand unification. Starting from a minimal model with multiple steps of symmetry breaking, we show that it generally prefers a high intermediate scale above 1014 GeV that is favored by observable primordial gravitational waves. The observed spectrum can potentially narrow the possible range of the cosmic string scale and restricts the unified couplings and the unification scale by requiring gauge coupling unification. As an indirect consequence of the high cosmic string scale, the monopole abundance places nontrivial constraints on the theory. These are complementary to the proton decay constraints and probe different facets of supersymmetric SOð10Þ unification theories. DOI: 10.1103/PhysRevD.104.035031 I. INTRODUCTION the dark matter [11,12]. Therefore, the supersymmetric SOð10Þ grand unified theory (GUT) is one of the most The structure of the Standard Model (SM) matter sector, compelling frameworks of physics beyond the SM.
    [Show full text]
  • Curvaton in Large Field Inflation
    ICRR-Report-676-2014-2 IPMU 14-0089 Prepared for submission to JCAP Curvaton in large field inflation Tomohiro Fujitaa;b Masahiro Kawasakic Shuichiro Yokoyamac aKavli Institute for the Physics and Mathematics of the Universe (Kavli IPMU), TODIAS, the University of Tokyo, 5-1-5 Kashiwanoha, Kashiwa, 277-8583, Japan bDepartment of Physics, University of Tokyo, Bunkyo-ku 113-0033, Japan cInstitute for Cosmic Ray Research, University of Tokyo, 5-1-5 Kashiwa-no-Ha, Kashiwa, Chiba, 277-8582, Japan E-mail: [email protected], [email protected], [email protected] Abstract. We comprehensively explore the quadratic curvaton models in the chaotic infla- tion. In the light of the BICEP2 result r ≈ 0:2, all model parameters and relevant observ- ables are computed. It is found the curvaton field value is constrained into a narrow range, −2 −1 0 −3 σ∗ = O(10 -10 ) and the running of the spectral index is ns & −10 . We show that if the curvaton is added, the models are heavily degenerated on the ns - r plane. However, in- troducing a new plane, the degeneracy can be resolved. To distinguish the curvaton models, 0 precise measurements of not only r but also ns and the tensor tilt nT are required. Keywords: inflation ArXiv ePrint: 1404.0951 arXiv:1404.0951v2 [astro-ph.CO] 4 Jun 2014 Contents 1 Introduction1 2 Implication for the curvaton scenario with the chaotic inflation2 2.1 Brief Review on the chaotic inflation2 2.2 Curvaton contribution to the tensor-to-scalar ratio and the spectral index3 2.3 Degeneracy on the ns-r plane5 3 Distinguish the models?6 3.1 Tensor tilt and the running of the spectral index of the curvature perturbations7 0 3.2 Resolution of the degeneracy on the ns-(nT =r) plane9 4 Comments on non-Gaussianity and the curvaton field value 10 5 Conclusion 12 A The other parameters 13 1 Introduction The inflation paradigm is accepted as an increasingly plausible scenario of the primordial universe.
    [Show full text]
  • Particle Physics Model of Curvaton Inflation in a Stable Universe
    PHYSICAL REVIEW D 101, 063533 (2020) Particle physics model of curvaton inflation in a stable universe † Zoltán P´eli* and István Nándori MTA-DE Particle Physics Research Group, H-4010 Debrecen, PO Box 105, Hungary ‡ Zoltán Trócsányi Institute for Theoretical Physics, ELTE Eötvös Loránd University, Pázmány P´eter s´etány 1/A, H-1117 Budapest, Hungary and MTA-DE Particle Physics Research Group, H-4010 Debrecen, PO Box 105, Hungary (Received 26 November 2019; revised manuscript received 17 February 2020; accepted 6 March 2020; published 27 March 2020) We investigate a particle physics model for cosmic inflation based on the following assumptions: (i) there are at least two complex scalar fields; (ii) the scalar potential is bounded from below and remains perturbative up to the Planck scale; (iii) we assume slow-roll inflation with maximally correlated adiabatic and entropy fluctuations 50–60 e-folds before the end of inflation. The energy scale of the inflation is set automatically by the model. Assuming also at least one massive right-handed neutrino, we explore the allowed parameter space of the scalar potential as a function of the Yukawa coupling of this neutrino. DOI: 10.1103/PhysRevD.101.063533 I. INTRODUCTION only open questions in particle physics—such as the origin of neutrino masses—but also those in cosmology. The standard model (SM) of elementary particle inter- One of the vigorously studied questions in our under- actions [1] has been proven experimentally to high pre- standing of the early universe is the physics of cosmic cision at the Large Electron Positrion Collider [2] and also inflation.
    [Show full text]
  • The Higgs Field and Early Universe Cosmology: a (Brief) Review
    The Higgs field and early universe cosmology: a (brief) review Bart Horn∗ Manhattan College, Department of Physics, New York, NY 10471, USA Abstract We review and discuss recent work exploring the implications of the Higgs field for early universe cosmology, and vice versa. Depending on the model under consideration the Higgs may be one of a few scalar fields determining the evolution and fate of the Universe, or the Higgs field may be connected to a rich sector of scalar moduli with complicated dynamics. In particular we look at the potential consequences of the Higgs field for inflation and its predictions, for the (meta)stability of the Standard Model vacuum, and for the existence of dynamical selection mechanisms in the landscape. 1 Introduction: implications of mh = 125 GeV The observation of the Higgs boson in 2012 [1, 2], with a mass of 125 GeV, marked the last piece of the Standard Model (SM) of particle physics to be discovered and inaugurated a new era of precision Higgs boson physics. Further experiments have measured the properties and couplings of the Higgs boson to increasing levels of precision and confirmed the consistency of arXiv:2007.10377v1 [hep-ph] 20 Jul 2020 the discovered particle with the predicted properties of the SM Higgs boson [3, 4, 5]. Ongoing and planned experiments at the energy and intensity frontier [6, 7, 8, 9] will measure the Higgs boson couplings to greater levels of precision and test the predictions of the SM at higher energies. Despite the many recent successes, however, many deep questions remain. So far the Large Hadron Collider has not observed any evidence for weak-scale supersymmetry or other particles beyond the Standard Model, leaving the physics that sets the scale of the Higgs boson mass unresolved.
    [Show full text]
  • Axionlike Origin of the Primordial Density Perturbation
    Axionlike Origin of the Primordial Density Perturbation Takeshi Kobayashi Kobayashi-Maskawa Institute for the Origin of Particles and the Universe, Nagoya University, Nagoya 464-8602, Japan E-mail: [email protected] We show that an axionlike field coupled to a new confining gauge group can generate the primordial density perturbation in the post-inflation universe. The axion decay constant and strong coupling scale are uniquely determined by observations of the density perturbation, which further suggest a temporal deconfinement of the gauge group after inflation. The resulting temperature-dependent axion potential, together with its periodic nature, gives rise to the red-tilted density perturbation, with a positive local-type non-Gaussianity of order unity. arXiv:2005.01741v2 [astro-ph.CO] 2 Jul 2020 1 Introduction The large-scale structure of our universe was seeded by tiny density fluctuations in the early universe. This picture of structure formation has been established by a variety of cosmological observations, which also revealed that the primordial density perturbation was adiabatic, nearly scale-invariant with a slight increase of the amplitude towards larger length scales (red-tilted), and nearly Gaussian. However, the physical origin of the density perturbation still remains a mystery. One possibility is that it was produced during cosmic inflation from fluctuations of the inflaton field. Alternatively, it could have been produced after inflation by another physical degree of freedom. In theories beyond the standard model of particle physics, the appearance of pseudo-Nambu- Goldstone bosons (PNGBs) of spontaneously broken global U(1) symmetries is ubiquitous. The most famous example is the QCD axion introduced for solving the strong CP problem [1].
    [Show full text]
  • Stability of a Tachyon Braneworld
    Stability of a tachyon braneworld Gabriel Germán,a Alfredo Herrera-Aguilar,b;c André Martorano Kuerten,a;d Dagoberto Malagón–Morejón,a and Roldão da Rochae aInstituto de Ciencias Físicas, Universidad Nacional Autónoma de México, Apartado Postal 48-3, 62251, Cuernavaca, Morelos, México bInstituto de Física, Benemérita Universidad Autónoma de Puebla, Apartado Postal J-48, 72570, Puebla, Puebla, México cInstituto de Física y Matemáticas, Universidad Michoacana de San Nicolás de Hidalgo, Ciudad Universitaria, CP 58040, Morelia, Michoacán, México dCentro de Ciências Naturais e Humanas, Universidade Federal do ABC, 09210-580, Santo André, SP, Brazil eCentro de Matemática, Computação e Cognição, Universidade Federal do ABC, 09210-580, Santo André, SP, Brazil E-mail: gabriel@fis.unam.mx, malagon@fis.unam.mx, [email protected], [email protected], [email protected] Abstract. Within the braneworld paradigm the tachyonic scalar field has been used to gener- ate models that attempt to solve some of the open problems that physics faces nowadays, both in cosmology and high energy physics as well. When these field configurations are produced by the interplay of higher dimensional warped gravity with some matter content, braneworld models must prove to be stable under the whole set of small fluctuations of the gravitational and matter fields background, among other consistency tests. Here we present a complete proof of the stability under scalar perturbations of tachyonic thick braneworlds with an em- bedded maximally symmetric 4D space-time, revealing its physical consistency. This family of models contains a recently reported tachyonic de Sitter thick braneworld which possesses a series of appealing properties.
    [Show full text]
  • Supersymmetric Dark Matter Candidates in Light of Constraints from Collider and Astroparticle Observables Jonathan Da Silva
    Supersymmetric Dark Matter candidates in light of constraints from collider and astroparticle observables Jonathan da Silva To cite this version: Jonathan da Silva. Supersymmetric Dark Matter candidates in light of constraints from collider and astroparticle observables. High Energy Physics - Phenomenology [hep-ph]. Université de Grenoble, 2013. English. NNT : 2013GRENY033. tel-00912650v2 HAL Id: tel-00912650 https://tel.archives-ouvertes.fr/tel-00912650v2 Submitted on 19 Jan 2017 HAL is a multi-disciplinary open access L’archive ouverte pluridisciplinaire HAL, est archive for the deposit and dissemination of sci- destinée au dépôt et à la diffusion de documents entific research documents, whether they are pub- scientifiques de niveau recherche, publiés ou non, lished or not. The documents may come from émanant des établissements d’enseignement et de teaching and research institutions in France or recherche français ou étrangers, des laboratoires abroad, or from public or private research centers. publics ou privés. THESE` Pour obtenir le grade de DOCTEUR DE L’UNIVERSITE´ DE GRENOBLE Specialit´ e´ : Physique Theorique´ Arretˆ e´ ministeriel´ : 7 aoutˆ 2006 Present´ ee´ par Jonathan DA SILVA These` dirigee´ par Genevieve` BELANGER´ prepar´ ee´ au sein du Laboratoire d’Annecy-le-Vieux de Physique Theorique´ (LAPTh) et de l’Ecole´ Doctorale de Physique de Grenoble Supersymmetric Dark Matter candidates in light of constraints from collider and astroparticle observables These` soutenue publiquement le 3 juillet 2013, devant le jury compose´ de : Dr. Rohini GODBOLE Professeur, CHEP Bangalore, Inde, Presidente´ Dr. Farvah Nazila MAHMOUDI Maˆıtre de Conferences,´ LPC Clermont, Rapporteur Dr. Ulrich ELLWANGER Professeur, LPT Orsay, Rapporteur Dr. Celine´ BŒHM Charge´ de recherche, Durham University, Royaume-Uni, Examinatrice Dr.
    [Show full text]
  • Fermi-Bounce Cosmology and the Fermion Curvaton Mechanism
    Dartmouth College Dartmouth Digital Commons Dartmouth Scholarship Faculty Work 5-18-2015 Fermi-Bounce Cosmology and the Fermion Curvaton Mechanism Stephon Alexander Dartmouth College Yi-Fu Cai McGill University Antonino Marcianò Fudan University Follow this and additional works at: https://digitalcommons.dartmouth.edu/facoa Part of the Cosmology, Relativity, and Gravity Commons Dartmouth Digital Commons Citation Alexander, Stephon; Cai, Yi-Fu; and Marcianò, Antonino, "Fermi-Bounce Cosmology and the Fermion Curvaton Mechanism" (2015). Dartmouth Scholarship. 2025. https://digitalcommons.dartmouth.edu/facoa/2025 This Article is brought to you for free and open access by the Faculty Work at Dartmouth Digital Commons. It has been accepted for inclusion in Dartmouth Scholarship by an authorized administrator of Dartmouth Digital Commons. For more information, please contact [email protected]. Physics Letters B 745 (2015) 97–104 Contents lists available at ScienceDirect Physics Letters B www.elsevier.com/locate/physletb Fermi-bounce cosmology and the fermion curvaton mechanism Stephon Alexander a, Yi-Fu Cai b, Antonino Marcianò c a Center for Cosmic Origins and Department of Physics and Astronomy, Dartmouth College, Hanover, NH 03755, USA b Department of Physics, McGill University, Montréal, QC, H3A 2T8, Canada c Center for Field Theory and Particle Physics & Department of Physics, Fudan University, 200433 Shanghai, China a r t i c l e i n f o a b s t r a c t Article history: A nonsingular bouncing cosmology can be achieved by introducing a fermion field with BCS condensation Received 23 February 2015 occurring at high energy scales. In this paper we are able to dilute the anisotropic stress near the Received in revised form 6 April 2015 bounce by means of releasing the gap energy density near the phase transition between the radiation Accepted 14 April 2015 and condensate states.
    [Show full text]
  • Higgs Cosmology
    Universidad Autonoma´ de Madrid Facultad de Ciencias Departamento de F´ısica Teorica´ HIGGS COSMOLOGY From the Early to the Late Universe Memoria de Tesis Doctoral realizada por Javier Rubio Pe~na presentada ante el Departamento de F´ısicaTe´orica de la Universidad Aut´onomade Madrid para la obtenci´ondel T´ıtulode Doctor en Ciencias. Tesis Doctoral dirigida por Juan Garc´ıa-Bellido Capdevila del Departamento de F´ısicaTe´oricay el I.F.T. de la Universidad Aut´onomade Madrid Madrid, Junio 2011. Abstract Inflation is nowadays a well established paradigm consistent with all the observations, related both to the background and to the matter perturbations in the Universe. The nature of the inflaton, as well as the overall picture of the transition between the inflationary and radiation eras, depend crucially on the different microphysics models in which inflation is embedded. The absence of a suitable candidate in the usual formulation of the Standard Model has motivated the search for alternatives in different extensions of the standard theory, as Supersymmetry or String Theory. Unfortunately, the strength of the couplings among the inflaton and the different matter species present in those models is generically unknown. This fact makes difficult the determination of the dominant reheating mechanism at the end of inflation and the associated efficiency of the reheating stage. In this PhD thesis we adopt a very different and reductionist point of view. We study the possibility of inflation to be a natural consequence of the Standard Model, rather than an indication of its weakness. The role of the inflaton is played by the Higgs boson, non-minimally coupled to gravity.
    [Show full text]
  • Curvaton Decay by Resonant Production of Higgs Bosons Rose Lerner Helsinki University and Helsinki Institute of Physics [email protected]
    Curvaton Decay by Resonant Production of Higgs Bosons Rose Lerner Helsinki University and Helsinki Institute of Physics [email protected] with Kari Enqvist and Daniel Figueroa DESY theory workshop 27th September 2012 ? ? + H ? For “electrically charged curvaton, see JCAP / arXiv:1207.1063 – Arttu Rajantie, Michela D’Onofrio, RL ? + H Outline Introduction What is the curvaton? Linking particle physics and cosmology Curvaton-Higgs coupling expectation difference: thermal background calculations and results Summary Precision cosmology 105 Planck fNL ≤ 5 ? Inflation Inflation is a period of accelerated expansion in the early universe • solves horizon problem • solves flatness problem • dilutes unwanted cosmological relics • generates perturbations that seed structure formation Image: M. Gasperini, G. Veneziano / Physics Reports 373 (2003) Inflation Inflation is a period of accelerated expansion in the early universe • solves horizon problem • solves flatness problem expansion • dilutes unwanted cosmological relics • generates perturbations that seed structure formation Image: M. Gasperini, G. Veneziano / Physics Reports 373 (2003) Inflation Inflation is a period of accelerated expansion in the early universe • solves horizon problem • solves flatness problem expansion • dilutes unwanted cosmological relics • generates perturbations that seed structure formation fluctuations Image: M. Gasperini, G. Veneziano / Physics Reports 373 (2003) Standard inflationary scenario: The scalar field φ is responsible for both the inflationary expansion
    [Show full text]