Neutrino Masses and the Structure of the Weak Gauge Boson
Total Page:16
File Type:pdf, Size:1020Kb
Load more
Recommended publications
-
International Centre for Theoretical Physics
IC/80/62 INTERNATIONAL CENTRE FOR THEORETICAL PHYSICS QUANTUM CHROMODYNAMICS A THEORY OF THE NUCLEAR FORCE U.S. Craigie INTERNATIONAL ATOMIC ENERGY AGENCY UNITED NATIONS EDUCATIONAL, SCIENTIFIC AND CULTURAL ORGANIZATION 1980 MIRAMARE-TRIESTE IC/8O/6E International Atomic Energy Agency sad United Rations Educational Scientific and Cultural Organization IBTEHHATIOHAL CEHTHB FOR THEORETICAL PHYSICS QUAHTUM CHROMODIHAMICS A THBORT OF TIffl KUCLEAK FORCE • H.S. Craigie tnterna.ttgp«l Centre for Theoretical Phyaics, Trieste, Italy, and Ietltuto IFuiotude dl Fisiea Kucleare, Sezlone dl Trieste, Italy. MHUHHB- TRIESTE June l?60 aliven at tJse Int#rM*iotial SuB»er College on Physics ana Seeds, Nathiagali,Pakistan, 1&-28 Jtm« 1980, EARLY ID"Ad ON T'KK NVCLrAR F'JRCK AiO Tire uMEKOENCE OF1 THE tJCD LAGRANGIAN Let us recap a little of the early ideas on the nuclear force. [n the AIMS s, nuclear structure was thought to be described in terms of elementary protons and neutrons, which formed an isospin doublet 5 =| P\ vith I, = -^ In these lectures I hope to give a brief outline of a possible theory for the proton aiui T = -rz for the neutron, where isospiti, i.e. SU{2) of the nuclear force and the strong interactions between elementary particles, invariance, vas the recognised symmetry of nuclear interactions at ttvit time. which ve suppose is responsible for nuclear matter. The theory I will be Further, the nuclear force between these nucleons was thought to be mediated by describing is known as quantum chromodynamics because of its association vith an elementary meson, which was seen to form an isotriplet (IT ,tt ,n ) because i new kind of nuclear charge called colour and its resemblance to quantum of its three charged states- If all these particles were elementary, then in electrodynamics. -
Conformal Symmetry in Field Theory and in Quantum Gravity
universe Review Conformal Symmetry in Field Theory and in Quantum Gravity Lesław Rachwał Instituto de Física, Universidade de Brasília, Brasília DF 70910-900, Brazil; [email protected] Received: 29 August 2018; Accepted: 9 November 2018; Published: 15 November 2018 Abstract: Conformal symmetry always played an important role in field theory (both quantum and classical) and in gravity. We present construction of quantum conformal gravity and discuss its features regarding scattering amplitudes and quantum effective action. First, the long and complicated story of UV-divergences is recalled. With the development of UV-finite higher derivative (or non-local) gravitational theory, all problems with infinities and spacetime singularities might be completely solved. Moreover, the non-local quantum conformal theory reveals itself to be ghost-free, so the unitarity of the theory should be safe. After the construction of UV-finite theory, we focused on making it manifestly conformally invariant using the dilaton trick. We also argue that in this class of theories conformal anomaly can be taken to vanish by fine-tuning the couplings. As applications of this theory, the constraints of the conformal symmetry on the form of the effective action and on the scattering amplitudes are shown. We also remark about the preservation of the unitarity bound for scattering. Finally, the old model of conformal supergravity by Fradkin and Tseytlin is briefly presented. Keywords: quantum gravity; conformal gravity; quantum field theory; non-local gravity; super- renormalizable gravity; UV-finite gravity; conformal anomaly; scattering amplitudes; conformal symmetry; conformal supergravity 1. Introduction From the beginning of research on theories enjoying invariance under local spacetime-dependent transformations, conformal symmetry played a pivotal role—first introduced by Weyl related changes of meters to measure distances (and also due to relativity changes of periods of clocks to measure time intervals). -
B2.IV Nuclear and Particle Physics
B2.IV Nuclear and Particle Physics A.J. Barr February 13, 2014 ii Contents 1 Introduction 1 2 Nuclear 3 2.1 Structure of matter and energy scales . 3 2.2 Binding Energy . 4 2.2.1 Semi-empirical mass formula . 4 2.3 Decays and reactions . 8 2.3.1 Alpha Decays . 10 2.3.2 Beta decays . 13 2.4 Nuclear Scattering . 18 2.4.1 Cross sections . 18 2.4.2 Resonances and the Breit-Wigner formula . 19 2.4.3 Nuclear scattering and form factors . 22 2.5 Key points . 24 Appendices 25 2.A Natural units . 25 2.B Tools . 26 2.B.1 Decays and the Fermi Golden Rule . 26 2.B.2 Density of states . 26 2.B.3 Fermi G.R. example . 27 2.B.4 Lifetimes and decays . 27 2.B.5 The flux factor . 28 2.B.6 Luminosity . 28 2.C Shell Model § ............................. 29 2.D Gamma decays § ............................ 29 3 Hadrons 33 3.1 Introduction . 33 3.1.1 Pions . 33 3.1.2 Baryon number conservation . 34 3.1.3 Delta baryons . 35 3.2 Linear Accelerators . 36 iii CONTENTS CONTENTS 3.3 Symmetries . 36 3.3.1 Baryons . 37 3.3.2 Mesons . 37 3.3.3 Quark flow diagrams . 38 3.3.4 Strangeness . 39 3.3.5 Pseudoscalar octet . 40 3.3.6 Baryon octet . 40 3.4 Colour . 41 3.5 Heavier quarks . 43 3.6 Charmonium . 45 3.7 Hadron decays . 47 Appendices 48 3.A Isospin § ................................ 49 3.B Discovery of the Omega § ...................... -
Astro-Ph/0410417V1 18 Oct 2004 Nwihteeaen Tbeconfigurations
Preon stars: a new class of cosmic compact objects J. Hansson∗ & F. Sandin† Department of Physics, Lule˚aUniversity of Technology, SE-971 87 Lule˚a, Sweden In the context of the standard model of particle physics, there is a definite upper limit to the density of stable compact stars. However, if a more fundamental level of elementary particles exists, in the form of preons, stability may be re-established beyond this limiting density. We show that a degenerate gas of interacting fermionic preons does allow for stable compact stars, with densities far beyond that in neutron stars and quark stars. In keeping with tradition, we call these objects “preon stars”, even though they are small and light compared to white dwarfs and neutron stars. We briefly note the potential importance of preon stars in astrophysics, e.g., as a candidate for cold dark matter and sources of ultra-high energy cosmic rays, and a means for observing them. PACS numbers: 12.60.Rc - 04.40.Dg - 97.60.-s - 95.35.+d I. INTRODUCTION The three different types of compact objects traditionally considered in astrophysics are white dwarfs, neutron stars (including quark and hybrid stars), and black holes. The first two classes are supported by Fermi pressure from their constituent particles. For white dwarfs, electrons provide the pressure counterbalancing gravity. In neutron stars, the neutrons play this role. For black holes, the degeneracy pressure is overcome by gravity and the object collapses indefinitely, or at least to the Planck density. arXiv:astro-ph/0410417v1 18 Oct 2004 The distinct classes of degenerate compact stars originate directly from the properties of gravity, as was made clear by a theorem of Wheeler and collaborators in the mid 1960s [1]. -
The Structure of Quarks and Leptons
The Structure of Quarks and Leptons They have been , considered the elementary particles ofmatter, but instead they may consist of still smaller entities confjned within a volume less than a thousandth the size of a proton by Haim Harari n the past 100 years the search for the the quark model that brought relief. In imagination: they suggest a way of I ultimate constituents of matter has the initial formulation of the model all building a complex world out of a few penetrated four layers of structure. hadrons could be explained as combina simple parts. All matter has been shown to consist of tions of just three kinds of quarks. atoms. The atom itself has been found Now it is the quarks and leptons Any theory of the elementary particles to have a dense nucleus surrounded by a themselves whose proliferation is begin fl. of matter must also take into ac cloud of electrons. The nucleus in turn ning to stir interest in the possibility of a count the forces that act between them has been broken down into its compo simpler-scheme. Whereas the original and the laws of nature that govern the nent protons and neutrons. More recent model had three quarks, there are now forces. Little would be gained in simpli ly it has become apparent that the pro thought to be at least 18, as well as six fying the spectrum of particles if the ton and the neutron are also composite leptons and a dozen other particles that number of forces and laws were thereby particles; they are made up of the small act as carriers of forces. -
Neutrino Mass Models: a Road Map
Neutrino Mass Models: a road map S.F.King School of Physics and Astronomy, University of Southampton, Southampton SO17 1BJ, UK E-mail: [email protected] Abstract. In this talk we survey some of the recent promising developments in the search for the theory behind neutrino mass and mixing, and indeed all fermion masses and mixing. The talk is organized in terms of a neutrino mass models road map according to which the answers to experimental questions provide sign posts to guide us through the maze of theoretical models eventually towards a complete theory of flavour and uni¯cation. 1. Introduction It has been one of the long standing goals of theories of particle physics beyond the Standard Model (SM) to predict quark and lepton masses and mixings. With the discovery of neutrino mass and mixing, this quest has received a massive impetus. Indeed, perhaps the greatest advance in particle physics over the past decade has been the discovery of neutrino mass and mixing involving two large mixing angles commonly known as the atmospheric angle θ23 and the solar angle θ12, while the remaining mixing angle θ13, although unmeasured, is constrained to be relatively small [1]. The largeness of the two large lepton mixing angles contrasts sharply with the smallness of the quark mixing angles, and this observation, together with the smallness of neutrino masses, provides new and tantalizing clues in the search for the origin of quark and lepton flavour. However, before trying to address such questions, it is worth recalling why neutrino mass forces us to go beyond the SM. -
Quark-Lepton Unification and Proton Decay
\\£ IC/80/72 INTERNATIONAL CENTRE FOR •2t i / -Tr/ THEORETICAL PHYSICS QUARK-LEPTON UNIFICATION AND PROTON DECAY Jogesh C. Pati and Abdus Salam INTERNATIONAL ATOMIC ENERGY AGENCY UNITED NATIONS EDUCATIONAL, SCIENTIFIC AND CULTURAL ORGANIZATION 1980 MIRAMARE-TRIESTE IC/60/72 QUABK-LEFTON UNIFICATION AND PROTON DECAY I. INTRODUCTION Jogesh C. Pati The hypothesis of prnncS unification servinR to unify all basic particles - quarks and leptons - and their force:; - weak, International Centre for Theoretical Physics, Trieste, Italy, electromagnetic as well as strong - stands at present primarily and on its aesthetic merits. It gives the flavour of synthesis in that it provides a rationale for the existence of quarks and Department of Physics, University of Maryland, College Park, leptons by assigning the two sets of particles to one multiplet + Maryland, USA, of a gauge symmetry G. It derives their forces through one principle-gauge unification. and With quarks and leptons in one multiplet of a local sponta- neously broken gauge symmetry G, baryon and lepton number conserv- ation cannot be absolute. This line of reasoning had led us to Abdiis Salam suggest in 1973 that the lightest baryon - the proton - must ultimately decay into leptons 2. Theoretical considerations International Centre for Theoretical Physics, Trieste, Italy, suggest a lifetime for the proton in the ran^e of 102° to 1033 a and years "5. Its decay modes and corresponding branching ratios depend In general upon the details of the structure of the symmetry Imperial College, London, England. Kroup and its breaking Dattern. What is worth noticing »t this Junction Is that studies of (i) proton decay modes, (il) n-n oscillation (iii) neutrinoless double 6-deeay and (iv) the weak angle T sin26y are perhaps the only effective tools we would have for sometiae to probe into the underlying design of grand unification. -
Quantum Gravity from the QFT Perspective
Quantum Gravity from the QFT perspective Ilya L. Shapiro Universidade Federal de Juiz de Fora, MG, Brazil Partial support: CNPq, FAPEMIG ICTP-SAIFR/IFT-UNESP – 1-5 April, 2019 Ilya Shapiro, Quantum Gravity from the QFT perspective April - 2019 Lecture 5. Advances topics in QG Induced gravity concept. • Effective QG: general idea. • Effective QG as effective QFT. • Where we are with QG?. • Bibliography S.L. Adler, Rev. Mod. Phys. 54 (1982) 729. S. Weinberg, Effective Field Theory, Past and Future. arXive:0908.1964[hep-th]; J.F. Donoghue, The effective field theory treatment of quantum gravity. arXive:1209.3511[gr-qc]; I.Sh., Polemic notes on IR perturbative quantum gravity. arXiv:0812.3521 [hep-th]. Ilya Shapiro, Quantum Gravity from the QFT perspective April - 2019 I. Induced gravity. The idea of induced gravity is simple, while its realization may be quite non-trivial, depending on the theory. In any case, the induced gravity concept is something absolutely necessary if we consider an interaction of gravity with matter and quantum theory concepts. I. Induced gravity from cut-off Original simplest version. Ya.B. Zeldovich, Sov. Phys. Dokl. 6 (1967) 883. A.D. Sakharov, Sov. Phys. Dokl. 12 (1968) 1040. Strong version of induced gravity is like that: Suppose that the metric has no pre-determined equations of motion. These equations result from the interaction to matter. Main advantage: Since gravity is not fundamental, but induced interaction, there is no need to quantize metric. Ilya Shapiro, Quantum Gravity from the QFT perspective April - 2019 And we already know that the semiclassical approach has no problems with renormalizability! Suppose we have a theory of quantum matter fields Φ = (ϕ, ψ, Aµ) interacting to the metric gµν . -
The Maxwell-Cassano Equations of an Electromagnetic-Nuclear Field Yields the Fermion & Hadron Architecture
ISSN: 2639-0108 Research Article Advances in Theoretical & Computational Physics The Maxwell-Cassano Equations of an Electromagnetic-nuclear Field Yields the Fermion & Hadron Architecture Claude Michael Cassano *Corresponding author Claude Michael Cassano, Santa Clara, California, USA; E-mail: cloudmichael@ Santa Clara, California, USA hotmail.com Submitted: 16 July 2019; Accepted: 23 July 2019; Published: 05 Aug 2019 Abstract The Helmholtzian operator and factorization, via the Maxwell-Cassano equations yields a fermion architecture table equivalent to that of the standard model and lead to linear transformation groups of the mesons and baryons, respectively; plus a straightforward elementary description of quark colour based on integral indices: 1,0,1, rather than the subjective, correlative explanation using: {R,G,B;Y} indexes. keywords: Helmholtzian, Klein-Gordon equation, electromag- where: netism, preon, elementary particles, standard model, elementary (2) particle, particle interactions, fermions, leptons, quarks, hadrons, mesons, baryons, Pauli matrices, Gell-Mann matrices, Hermitian (3) matrices, Lie algebra, su(2), Yukawa potential Similarly, mass-generalized electric and magnetic potentials for the Introduction Helmholtzian operator factorization : Using the principles of the analysis of a linear function of a linear variable [1], constuctive algebras developed using the weighted matrix product [2] leads to the d’Alembertian operator and it’s factorization [3], and a space with all smooth functions satisfying Maxwell’s equations [4] [5] [6] [7]. This leads to the Helmholtzian operator and factorization[8], and a space in which all smooth functions satisfy the Maxwell-Cassano equations[9] (which generalizes both Maxwell’s equations and the Dirac equation [10] [11] [12]) - a linearization of the Klein-Gordon equations [13] [14] [12]. -
Lecture 2 - Energy and Momentum
Lecture 2 - Energy and Momentum E. Daw February 16, 2012 1 Energy In discussing energy in a relativistic course, we start by consid- ering the behaviour of energy in the three regimes we worked with last time. In the first regime, the particle velocity v is much less than c, or more precisely β < 0:3. In this regime, the rest energy ER that the particle has by virtue of its non{zero rest mass is much greater than the kinetic energy T which it has by virtue of its kinetic energy. The rest energy is given by Einstein's famous equation, 2 ER = m0c (1) So, here is an example. An electron has a rest mass of 0:511 MeV=c2. What is it's rest energy?. The important thing here is to realise that there is no need to insert a factor of (3×108)2 to convert from rest mass in MeV=c2 to rest energy in MeV. The units are such that 0.511 is already an energy in MeV, and to get to a mass you would need to divide by c2, so the rest mass is (0:511 MeV)=c2, and all that is left to do is remove the brackets. If you divide by 9 × 1016 the answer is indeed a mass, but the units are eV m−2s2, and I'm sure you will appreciate why these units are horrible. Enough said about that. Now, what about kinetic energy? In the non{relativistic regime β < 0:3, the kinetic energy is significantly smaller than the rest 1 energy. -
Pages from C13-03-02 3.Pdf
The GIM Mechanism: origin, predictions and recent uses Luciano Maiani CERN, Geneva, Switzerland Dipartimento di Fisica, Universita di Roma La Sapienza, Roma, Italy The GIM Mechanism was introduced by Sheldon L. Glashow, John Iliopoulos and Luciano Maiani in 1970) to explain the suppression of Delta S=l, 2 neutral current processes and is an important element of the unified theories of the weak and electromagnetic interactions. Origin, predictions and uses of the GIM Mechanism are illustrated. Flavor changing neutral current processes (FCNC) represent today an important benchmark for the Standard Theory and give strong limitations to theories that go beyond ST in the fewTe V region. Ideas on the ways constraints on FCNC may be imposed are briefly described. 1 Setting the scene The final years of the sixties marked an important transition period for the physics of elementary particles. Two important discoveries made in the early sixties, quarks and Cabibbo theory, had been consolidated by a wealth of new data and there was the feeling that a more complete picture of the strong and of the electro-weak interactions could be at hand. The quark model of hadrons introduced by M. Gell-Mann 1 and G. Zweig2 explained neatly the spectrum of the lowest lying mesons and baryons as qij and qqq states, respectively, with: (1) and electric charges Q 2/3 1/3 /3 respectively. 1 Doubts persisted on= quarks, - being, - real, physical entities or rather a simple mathematical tool to describe hadrons. This was due to the symmetry puzzle, namely the fact that one had to assume an overall symmetric configuration of the three quarks to describe the spin-charge structure of the baryons, rather than the antisymmetric configuration required by the fermion nature of physical, spin 1/2, quark$'. -
A Fermi National Accelerator Laboratory
a Fermi National Accelerator Laboratory FERMILAB-Pub-83/l&THY January, 1983 Composite Model with Confining SU(N) x SU(2)L x SU(2)K Hypercolor Carl H. Albright Fermi National Accelerator Laboratory P.O. Box 500, Batavia, Illinois 60510 and Department of Physics, Northern Illinois University* DeKalb, Illinois 60115 ABSTRACT A model of composite quarks and leptons is constructed with confining SU(N) x SU(2jL x SU(2)R hypercolor interactions such that only standard quark and lepton families appear in global SU(2)L x SU(2)K doublets. Several generations are admitted by the anomaly-matching conditions and labeled by a discrete axial symmetry. The SU(N) interactions are N independent and play the role Of technicolor. Three conserved U(l)" charges identified with Q, B - L and B + L prohibit qqq + Lc transitions. 3 Oparatrd by Unlvsrsitiae Research Association Inc. under contract with the United States Department of Energy -2- FERMILAB-Pub-83/16-THY With little or no support from the experimental realm, an extensive literature fl on the subject of composite quarks and leptons has emerged over the past few years. Many of the papers are based on the pioneering work of 't Hooft who formulated several criteria which composite models should satisfy in order to explain why quarks and leptons are nearly massless on the large energy scale where the hypercolor forces become sufficiently strong to bind the massless preons together. General searches for candidate preon models have been carried out, or specfific models themselves have been proposed, in which the fundamental preons are either all spinors or spinors and scalars and the weak gauge fields are either fundamental or composite.