DOCSLIB.ORG

Higgs Cosmology

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read 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. No new degrees of freedom apart from those already present in the electroweak theory are initially added. The non-minimal coupling rescues the Higgs field from the known difficulties for generating inflation, being its value determined by cosmological observations. The novelty and great advantage of the model is precisely its connection with a well-known microphysical mechanism, hopefully accessible in the present accelerator experiments. All the couplings among the Higgs and the Standard Model particles are known at the electroweak scale and can be extrapolated to the reheating era through the renormalization group equations. For the first time, the initial conditions of the hot Big Bang can be potentially determined, without invoking new speculative physics beyond the electroweak scale. Some modest extensions of the simplest Higgs Inflation model, based on scale invariance and Unimodular Gravity, are able to accommodate not only the early but also the late time acceleration of the Universe. Contrary to other beyond the Standard Model theories, they introduce just an extra degree of freedom, the dilaton, which plays however a central role, tracking the present expansion rate of the Universe. The close connection between the inflationary and dark energy dominated eras leads to highly non-trivial consistency relations between the spectral tilt of CMB anisotropies and the present equation of state of dark energy. Resumen Inflaci´ones a d´ıa de hoy un paradigma bien establecido consistente con todas las obser- vaciones. Su naturaleza, as´ı como los aspectos globales de la transici´onentre el estado inflacionario y la ´epoca dominada por materia, dependen en gran medida de los diferentes modelos microsc´opicosen los que se implementa. La ausencia de un candidato a inflat´onen el Modelo Est´andar ha motivado la busqueda de alternativas en extensiones de esta teor´ıa, como Supersimetr´ıao teor´ıa de cuerdas. Desafortunadamente, desconocemos la intensidad de los acoplos entre el inflaton y el contenido de materia de dicho modelos. Este hecho dificulta la determinaci´ondel mecanismo de recalentamiento dominante y su eficiencia. En esta t´esis abordaremos el problema desde un punto de vista muy diferente y reduccionista. Estudiare- mos el inflat´onno como una indicaci´onde la debilidad del modelo est´andar, sino como una consecuencia natural del mismo. Ser´ael propio campo de Higgs, ya presente en el Modelo Est´andar,el que juege el papel de inflat´onmediante un acoplo no m´ınimoa gravedad. No se incorporar´aninicialmente nuevos grados de libertad, m´asall´ade los ya presentes en la teor´ıaelectrod´ebil.La novedad, y al mismo tiempo gran ventaja, de este modelo es precisa- mente su conexi´oncon un mecanismo microf´ısicobien conocido, y que podr´ıaser accesible en los aceleradores de part´ıculasactuales. Todos los acoplos entre el Higgs y las part´ıculas del Modelo Est´andarse conocen a la escala electrod´ebil, pudi´endoseextrapolar a la era del recalentamiento mediante las ecuaciones del grupo de renormalizaci´on.La determinaci´onde las condiciones iniciales del Big Bang es por primera vez posible sin la necesidad de invocar nueva y especulativa f´ısicam´asall´ade la escala electrod´ebil. Algunas extensiones relativa- mente modestas de Higgs Inflation, basadas en invarianza de escala y gravedad unimodular, son capaces de acomodar no s´oloel estad´ıo inflacionario, sino tambi´enla aceleraci´ondel universo actual. Contrariamente a otros modelos, estas extensiones introducen solamente un grado de libertad adicional, el dilat´on,que juega sin embargo un papel central en el modelo, determinando la tasa de expansi´onactual del mismo. La gran conexi´onentre el proceso inflacionario y la energ´ıaoscura da lugar a relaciones de consistencia altamente no triviales entre el tilte espectral de las anisotrop´ıasdel CMB y la ecuaci´onde estado de energ´ıaoscura. A mi familia, que me lo ha dado todo. Acknowledgements A todos los que la presente vieren y entendieren. Inicio de las Leyes Org´anicas. I am indebted to many people for their help and support during the last few years. I am particularly thankful to my supervisor Juan Garc´ıa-Bellidofor sharing with me his insight in the interplay between particle physic and cosmology. My view of understanding the physics, my critical view of it as well as maybe my prejudices are clearly influenced by him. I would like also to thank all the members of SISSA-Trieste, MPI-Munich and EPFL-Lausanne for the hospitality and very pleasant working environment during the development of part of the research presented in this thesis. I am particularly thankful to Stefano Liberati, Ignacio Cirac and Mikhail Shaposhnikov for allowing me to visit those institutions and for guiding me in the exploration of their very diverse disciplines. Great thanks to Daniel Zenhausern and Daniel G. Figueroa for the fruitful and enjoyable collaborations we had in Madrid and Lausanne respectively. Thanks also to Anupam Mazumdar, Jose Pedro Mimoso and Stefano Liberati for their comments and suggestions about this manuscript and for bringing to my attention references which would have otherwise missed in the large literature. Finally I would like to mention the efficient secretarial staff of the Department and Institute of Theoretical Physics for all the bureaucratic help along the past few years. In the most personal part of these acknowledgments, I would like to thank my co- PhD students and friends in Madrid: Roberto, Bea, Domenico, Luis, Norberto, Jaime, Joao, Brian, Ana, Josu, Javis, Migueles and many others who will surely forgive me not to include their name in this long list. Among them I would like to convey my special affection to Fran and Pilar, for all we have shared during these years and for helping me so much with the technicalities of this thesis. In the past few years, I met a lot of people in different workshops and meetings and some of them have also become good friends. Thanks Hector, Aurelio, Guillem, Noela, Marco, Julien, Iker for all the good moments we lived. Among my carissimi amici out of the Institute deserve a special mention Cristina and Jose, for being there in all my bad moments before, during and hopefully after the preparation of this thesis. They are a central part of my life. Great friends are also Mar´ıay Pedro, with whom I spent one of the best vacations of my life and hopefully many others. Thanks Mar´ıafor that wonderful piece of advise that you gave me in Zamora. Last, but not least, I wish to thank my fathers Tino and Emilia, my sister Beatriz and my lovely grandparents for their invaluable and unconditional support along all my life. Everything I am I owe to you. Qu´ete parece desto, Sancho? - dijo Don Quijote - Bien podr´an los encantadores quitarme la ventura, pero el esfuerzo y el ´animo,ser´aimposible. Segunda parte del Ingenioso Caballero Don Quijote de la Mancha Miguel de Cervantes - Buena est´a- dijo Sancho -; f´ırmelavuestra merced. No es menester firmarla -dijo Don Quijote-, sino solamente poner mi r´ubrica. Primera parte del Ingenioso Caballero Don Quijote de la Mancha Miguel de Cervantes Declaration The material presented in this PhD thesis is based on original contributions done during the course of my PhD studies. In particular the results scattered through Chapters2,3 and5 are based on Ref. 2 on the list below, while the main results of Chapter4 are contained in Ref. 1 This last chapter is also influenced by Ref. 3. although the details have not been included for being yet work in progress. Chapter1 describe the motivation of the Higgs-driven inflationary models considered in this PhD thesis, while a summary of the main results of this thesis is presented in Chapter6. The appendicesA andB contains mainly non-original contributions included to clarify some technical aspects of this PhD thesis. On the other hand the results presented in AppendixC constitute also original material. 1. Preheating in the Standard Model with the Higgs-Inflaton Coupled to Gravity. Juan Garcia-Bellido, Daniel G. Figueroa and Javier Rubio Phys. Rev. D 79 063531 (2009) 2. Higgs Cosmology: From the Early to the Late Universe.
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]
  • Who Is the Inflaton ?
    View metadata, citation and similar papers at core.ac.uk Who is the Inflaton ? brought to you by CORE provided by CERN Document Server R. Brout Service de Physique Th´eorique, Universit´e Libre de Bruxelles, CP 225, Bvd. du Triomphe, B-1050 Bruxelles, Belgium, (email: [email protected]). It is proposed that the inflaton field is proportional to the fluctuation of the number density of degrees of freedom of the fields of particle physics. These possess cut-off momenta at O (mP lanck), but this fluctuates since the fields propagate in an underlying space-time transplanckian substratum. If the latter is modeled as an instanton fluid in the manner of Hawking's space-time foam, then this identification, in the rough, is equivalent to the inflaton being the fluctuation of the spatial density of instantons. This interpretation is suggested by Volovik's analogy between space-time and the superfluid. (However, unlike for the latter, one cannot argue from the analogy that the cosmological constant vanishes). In our interpretation Linde's phenomenology of inflation takes on added luster in this way to look at things, since inflation and particle production follow quite naturally from familiar physical concepts operating on a "cisplanckian" level. I. INTRODUCTION In his lectures on cosmology at Erice 1999, Professor E. Kolb in extolling the virtues of the inflaton scenario of inflation closed his inspiring lesson with the resounding question : "Who is the inflaton ?" In the foregoing I shall hazard an answer. My intention, in the present paper, is to introduce more a theoretical framework of conjectural character than any quantitative realization.
    [Show full text]
  • Supersymmetry and Inflation
    Supersymmetry and Inflation Sergio FERRARA (CERN – LNF INFN) July 14 , 2015 Fourteenth Marcel Grossmann Meeting, MG14 University of Rome “La Sapienza”, July 12-18 2015 S. Ferrara - MG14, U. Rome "La Sapienza" 1 July 2015 Contents 1. Single field inflation and Supergravity embedding 2. Inflation and Supersymmetry breaking 3. Minimal models for inflation: a. One chiral multiplet (sgoldstino inflation) b. Two chiral multiplets: T (inflaton), S (sgoldstino) 4. R + R2 Supergravity 5. Nilpotent inflation (sgoldstino-less models) 6. Models with two Supersymmetry breaking scales S. Ferrara - MG14, U. Rome "La Sapienza" July 2015 2 We describe approaches to inflaton dynamics based on Supergravity, the combination of Supersymmetry with General Relativity (GR). Nowadays it is well established that inflationary Cosmology is accurately explained studying the evolution of a single real scalar field, the inflaton, in a Friedmann, Lemaître, Robertson, Walker geometry. A fundamental scalar field, which described the Higgs particle, was also recently discovered at LHC, confirming the interpretation of the Standard Model as a spontaneously broken phase (BEH mechanism) of a non-abelian Yang-Mills theory (Brout, Englert, Higgs, 1964). S. Ferrara - MG14, U. Rome "La Sapienza" July 2015 3 There is then some evidence that Nature is inclined to favor, both in Cosmology and in Particle Physics, theories which use scalar degrees of freedom, even if in diverse ranges of energy scales. Interestingly, there is a cosmological model where the two degrees of freedom, inflaton and Higgs, are identified, the Higgs inflation model (Bezrukov, Shaposhnikov, 2008), where a non-minimal coupling 2 h R of the Higgs field h to gravity is introduced.
    [Show full text]
  • Arxiv:2107.01683V1 [Hep-Ph] 4 Jul 2021 Ai Prxmto Nte2 Oe Hog H Higgs-Dilat the field
    Communications in Physics, Vol. 0, No. 0 (0), pp. 1-15 CONSTRAINT ON THE HIGGS-DILATON POTENTIAL VIA WARM INFLATION IN TWO-TIME PHYSICS VO QUOC PHONG AND NGO PHUC DUC LOC Department of Theoretical Physics, University of Science, Ho Chi Minh City, Vietnam Vietnam National University, Ho Chi Minh City, Vietnam Abstract. Within the SP (2, R) symmetry, the Two-time model (2T model) has six dimensions with two dimensions of time and the dilaton field that can be identified as inflaton in a warm inflation scenario with potential of the form ∼ φ4. From that consideration, we derive the range of parameters for the Higgs-Dilaton potential, the coupling constant between Higgs and Dialton − (α) is lager than 1.598 or smaller than 2.13 × 10 7 when the mass of Dilaton is lager than 200 GeV. Therefore, the 2T-model indirectly suggests that extra-dimension can also be a source of inflation. I. Introduction The 2T model [1, 2, 3, 4, 5, 6, 7] could be a well known choice. The model presents us with an unusual vision of time that advances on a plane, i.e., it has two dimensions of time. This model’s spontaneous symmetry breakdown is also different from the SM’s. The 2T physics is a combination of the standard model’s extended theory and the space-time or gravity theory. This theory has proposed expanding the number of spacetime dimensions to represent the whole cosmos, as well as the introduction of dilaton and its properties, for more than a decade (since 2008).
    [Show full text]
  • Prospects for Measurements with Strange Hadrons at Lhcb
    Prospects for measurements with strange hadrons at LHCb A. A. Alves Junior1, M. O. Bettler2, A. Brea Rodr´ıguez1, A. Casais Vidal1, V. Chobanova1, X. Cid Vidal1, A. Contu3, G. D'Ambrosio4, J. Dalseno1, F. Dettori5, V.V. Gligorov6, G. Graziani7, D. Guadagnoli8, T. Kitahara9;10, C. Lazzeroni11, M. Lucio Mart´ınez1, M. Moulson12, C. Mar´ınBenito13, J. Mart´ınCamalich14;15, D. Mart´ınezSantos1, J. Prisciandaro 1, A. Puig Navarro16, M. Ramos Pernas1, V. Renaudin13, A. Sergi11, K. A. Zarebski11 1Instituto Galego de F´ısica de Altas Enerx´ıas(IGFAE), Santiago de Compostela, Spain 2Cavendish Laboratory, University of Cambridge, Cambridge, United Kingdom 3INFN Sezione di Cagliari, Cagliari, Italy 4INFN Sezione di Napoli, Napoli, Italy 5Oliver Lodge Laboratory, University of Liverpool, Liverpool, United Kingdom, now at Universit`adegli Studi di Cagliari, Cagliari, Italy 6LPNHE, Sorbonne Universit´e,Universit´eParis Diderot, CNRS/IN2P3, Paris, France 7INFN Sezione di Firenze, Firenze, Italy 8Laboratoire d'Annecy-le-Vieux de Physique Th´eorique , Annecy Cedex, France 9Institute for Theoretical Particle Physics (TTP), Karlsruhe Institute of Technology, Kalsruhe, Germany 10Institute for Nuclear Physics (IKP), Karlsruhe Institute of Technology, Kalsruhe, Germany 11School of Physics and Astronomy, University of Birmingham, Birmingham, United Kingdom 12INFN Laboratori Nazionali di Frascati, Frascati, Italy 13Laboratoire de l'Accelerateur Lineaire (LAL), Orsay, France 14Instituto de Astrof´ısica de Canarias and Universidad de La Laguna, Departamento de Astrof´ısica, La Laguna, Tenerife, Spain 15CERN, CH-1211, Geneva 23, Switzerland 16Physik-Institut, Universit¨atZ¨urich,Z¨urich,Switzerland arXiv:1808.03477v2 [hep-ex] 31 Jul 2019 Abstract This report details the capabilities of LHCb and its upgrades towards the study of kaons and hyperons.
    [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]
  • JHEP05(2010)010 , 6 − Ing Springer and 10 May 4, 2010 9 : April 19, 2010 − : Tic Inflationary December 3, 2009 : Published Lar Potential, and No S
    Published for SISSA by Springer Received: December 3, 2009 Accepted: April 19, 2010 Published: May 4, 2010 Light inflaton hunter’s guide JHEP05(2010)010 F. Bezrukova and D. Gorbunovb aMax-Planck-Institut f¨ur Kernphysik, P.O. Box 103980, 69029 Heidelberg, Germany bInstitute for Nuclear Research of the Russian Academy of Sciences, 60th October Anniversary prospect 7a, Moscow 117312, Russia E-mail: [email protected], [email protected] Abstract: We study the phenomenology of a realistic version of the chaotic inflationary model, which can be fully and directly explored in particle physics experiments. The inflaton mixes with the Standard Model Higgs boson via the scalar potential, and no additional scales above the electroweak scale are present in the model. The inflaton-to- Higgs coupling is responsible for both reheating in the Early Universe and the inflaton production in particle collisions. We find the allowed range of the light inflaton mass, 270 MeV . mχ . 1.8 GeV, and discuss the ways to find the inflaton. The most promising are two-body kaon and B-meson decays with branching ratios of orders 10−9 and 10−6, respectively. The inflaton is unstable with the lifetime 10−9–10−10 s. The inflaton decays can be searched for in a beam-target experiment, where, depending on the inflaton mass, from several billions to several tenths of millions inflatons can be produced per year with modern high-intensity beams. Keywords: Cosmology of Theories beyond the SM, Rare Decays ArXiv ePrint: 0912.0390 Open Access doi:10.1007/JHEP05(2010)010 Contents 1 Introduction 1 2 The model 3 3 Inflaton decay palette 6 4 Inflaton from hadron decays 10 JHEP05(2010)010 5 Inflaton production in particle collisions 12 6 Limits from direct searches and predictions for forthcoming experiments 14 7 Conclusions 16 A The νMSM extension 16 1 Introduction In this paper we present an example of how (low energy) particle physics experiments can directly probe the inflaton sector (whose dynamics is important at high energies in the very Early Universe).
    [Show full text]
  • Higgs Inflation
    Higgs inflation Javier Rubio Institut fur¨ Theoretische Physik, Ruprecht-Karls-Universitat¨ Heidelberg, Philosophenweg 16, 69120 Heidelberg, Germany —————————————————————————————————————————— Abstract The properties of the recently discovered Higgs boson together with the absence of new physics at collider experiments allows us to speculate about consistently extending the Standard Model of particle physics all the way up to the Planck scale. In this context, the Standard Model Higgs non- minimally coupled to gravity could be responsible for the symmetry properties of the Universe at large scales and for the generation of the primordial spectrum of curvature perturbations seeding structure formation. We overview the minimalistic Higgs inflation scenario, its predictions, open issues and extensions and discuss its interplay with the possible metastability of the Standard Model vacuum. —————————————————————————————————————————— arXiv:1807.02376v3 [hep-ph] 13 Mar 2019 Email: [email protected] 1 Contents 1 Introduction and summary3 2 General framework7 2.1 Induced gravity . .7 2.2 Higgs inflation from approximate scale invariance . .8 2.3 Tree-level inflationary predictions . 11 3 Effective field theory interpretation 14 3.1 The cutoff scale . 14 3.2 Relation between high- and low-energy parameters . 16 3.3 Potential scenarios and inflationary predictions . 17 3.4 Vacuum metastability and high-temperature effects . 21 4 Variations and extensions 22 4.1 Palatini Higgs inflation . 23 4.2 Higgs-Dilaton model . 24 5 Concluding remarks 26 6 Acknowledgments 26 2 1 Introduction and summary Inflation is nowadays a well-established paradigm [1–6] able to explain the flatness, homogene- ity and isotropy of the Universe and the generation of the primordial density fluctuations seeding structure formation [7–10].
    [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]
  • Pos(Leptonphoton2015)030 ∗ [email protected] Speaker
    Rare Decays of Heavy Mesons PoS(LeptonPhoton2015)030 Gaia LANFRANCHI∗ (on behalf of the LHCb collaboration) Laboratori Nazionali di Frascati, INFN E-mail: [email protected] Rare decays of heavy mesons provide some of the most promising approaches for testing the Standard Model with high level of accuracy. In this paper, the status and prospects in the field are reviewed, with a focus on the measurements performed by the LHCb, CMS and ATLAS collaborations at the Large Hadron Collider at CERN. International Symposium on Lepton Photon Interactions at High Energies XXVII International Symposium on Lepton Photon Interactions at High Energies 17-22 August 2015 Ljubljana,University Slovenia of Ljubljana, Slovenia ∗Speaker. c Copyright owned by the author(s) under the terms of the Creative Commons Attribution-NonCommercial-NoDerivatives 4.0 International License (CC BY-NC-ND 4.0). http://pos.sissa.it/ Rare Decays of Heavy Mesons Gaia LANFRANCHI 1. Introduction The Standard Model (SM) of particle physics cannot be the ultimate theory, as it is incomplete and contains too many free parameters, such as the fermion masses and the quark mixing angles. The pattern of these parameters could be governed by a hidden mechanism yet to be discovered, and so the SM would be a low-energy effective theory of a more fundamental theory that would be superseded by a higher energy scale, expected in the TeV region and accessible at the Large Hadron Collider (LHC). This would imply new symmetries, particles, dynamics, and flavor structure (New Physics, NP) that can be discovered either directly or indirectly.
    [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]