What Comes Beyond the Standard Models Bled, July 11–19, 2016
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Chaos, Scaling and Existence of a Continuum Limit in Classical Non-Abelian Lattice Gauge Theory
LA-UR- 9 6 " 4 43"6" Los Alamos National Laboratory is operated by the University of Caiifomia for the United States Department of Energy under contract W-7405-ENG-36 TITLE: CHAOS, SCALING AND EXISTENCE OF A CONTINUUM Q&TJ LIMIT IN CLASSICAL NON-ABELIAN LATTICE GAUGE THEORY AUTHOR(S): Holger Nielsen, Niels Bohr Institute Hans Rugh, Universty of Warwick Svend Rugh, T-6 SUBMITTED TO: 28TH INTERNATIONAL CONFERENCE ON HIGH ENERGY PHYSICS, WARSAW POLAND, JULY 1996 By acceptance of this article, the publisher recognizes that the U.S. Government retains a nonexclusive, royalty-free license to publish or reproduce the published form of this contribution, or to allow others to do so, for U.S. Government purposes. The Los Alamos National Laboratory requests that the publisher identify this article as work performed under the auspices of the U.S. Department of Energy. Los Alamos National Laboratory L< Los Alamos, New Mexico 87545 FORM NO. 836 R4 ST. NO. 2629 5/81 DISTRIBUTION OF THIS DOCUMENT IS UNLIMITED DISCLAIMER Portions of this document may be illegible in electronic image products. Images are produced from the best available original document DISCLAIMER This report was prepared as an account of work sponsored by an agency of the United States Government Neither the United States Government nor any agency thereof, nor any of their employees, makes any warranty, express or implied, or assumes any legal liability or responsibility for the accuracy, completeness, or use- fulness of any information, apparatus, product, or process disclosed, or represents that its use would not infringe privately owned rights. -
Current Perspectives on Dark Matter
Cosmological Signatures of a Mirror Twin Higgs Zackaria Chacko University of Maryland, College Park Curtin, Geller & Tsai Introduction The Twin Higgs framework is a promising approach to the naturalness problem of the Standard Model (SM). In Mirror Twin Higgs models, the SM is extended to include a complete mirror (“twin”) copy of the SM, with its own particle content and gauge groups. The SM and its twin counterpart are related by a discrete Z2 “twin” symmetry. Z2 SMA SMB The mirror particles are completely neutral under the SM strong, weak and electromagnetic forces. Only feel gravity. In Mirror Twin Higgs models, the one loop quadratic divergences that contribute to the Higgs mass are cancelled by twin sector states that carry no charge under the SM gauge groups. Discovery of these states at LHC is therefore difficult. May explain null results. The SM and twin SM primarily interact through the Higgs portal. This interaction is needed for cancellation of quadratic divergences. After electroweak symmetry breaking, SM Higgs and twin Higgs mix. • Higgs couplings to SM states are suppressed by the mixing. • Higgs now has (mixing suppressed) couplings to twin states. A soft breaking of the Z2 symmetry ensures that 퐯B, the VEV of the twin Higgs, is greater than 퐯A, the VEV of the SM Higgs. The mixing angle ~ 퐯A/퐯B. Higgs measurements constrain 퐯A/퐯B ≤ ퟏ/ퟑ. Twin fermions are heavier than SM fermions by a factor of 퐯B/퐯A . Naturalness requires 퐯A/퐯B ≥ ퟏ/ퟓ. (Twin top should not be too heavy.) The Higgs portal interaction has implications for cosmology. -
Signs of Dark Matter May Point to Mirror Matter Candidate 27 April 2010, by Lisa Zyga
Signs of dark matter may point to mirror matter candidate 27 April 2010, by Lisa Zyga (PhysOrg.com) -- Dark matter, which contains the At first, mirror matter may sound a bit like antimatter "missing mass" that's needed to explain why (which is ordinary matter with an opposite charge). galaxies stay together, could take any number of In both theories, the number of known particles forms. The main possible candidates include would double. However, while antimatter interacts MACHOS and WIMPS, but there is no shortage of very strongly with ordinary matter, annihilating itself proposals. Rather, the biggest challenge is finding into photons, mirror matter would interact very some evidence that would support one or more of weakly with ordinary matter. For this reason, some these candidates. Currently, more than 30 physicists have speculated that mirror particles experiments are underway trying to detect a sign of could be candidates for dark matter. Even though dark matter. So far, only two experiments claim to mirror matter would produce light, we would not see have found signals, with the most recent it, and it would be very difficult to detect. observations coming just a month ago. Now, physicist Robert Foot from the University of However, mirror matter would not be impossible to Melbourne has shown that the results of these two detect, and Foot thinks that the DAMA experiment experiments can be simultaneously explained by and the CoGeNT experiment may have detected an intriguing dark matter candidate called mirror mirror matter. In DAMA, scientists observed a piece matter. of sodium iodide, which should generate a photon when struck by a dark matter particle. -
Pos(CORFU2019)049 ∗ -Ray Excess
Several degenerate vacua and a model for Dark Matter in the pure Standard Model PoS(CORFU2019)049 Holger Bech Nielsen∗ Niels Bohr Institute, Blegdamsvej 15 -21, Copenhagen E-mail: [email protected] Colin D. Froggatt Glasgow University E-mail: [email protected] We return to a model of ours for what the dark matter can be with the property that it is compatible with the Standard Model alone. The only genuine new physics is a principle imposing restrictions on the parameters/couplings in the Standard Model. They are required to lead to several vacua being degenerate in energy density with each other. We especially look for some of the signals from the dark matter, which are not just gravitational: The 3.55 keV X-ray radiation, the positron excess and further g-ray excess. The picture of ours for dark matter has it being cm-size pearls of 100000 ton mass in order of magnitude. Corfu Summer Institute 2019 "School and Workshops on Elementary Particle Physics and Gravity" (CORFU2019) 31 August - 25 September 2019 Corfu, Greece ∗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/ Dark matter, pure S.M. Holger Bech Nielsen 1. Introduction Several degenerate vacua and a model for Dark Matter in the pure Standard Model We believe in the pure Standard Model further up in energy than most physicists, except for see-saw neutrinos and the baryon number excess for which we accept the need for new physics: • No new fundamental particles, except see-saw neutrinos and possibly particles almost at the Planck scale; but we shall not talk about such high energies today. -
Roman Jackiw: a Beacon in a Golden Period of Theoretical Physics
Roman Jackiw: A Beacon in a Golden Period of Theoretical Physics Luc Vinet Centre de Recherches Math´ematiques, Universit´ede Montr´eal, Montr´eal, QC, Canada [email protected] April 29, 2020 Abstract This text offers reminiscences of my personal interactions with Roman Jackiw as a way of looking back at the very fertile period in theoretical physics in the last quarter of the 20th century. To Roman: a bouquet of recollections as an expression of friendship. 1 Introduction I owe much to Roman Jackiw: my postdoctoral fellowship at MIT under his supervision has shaped my scientific life and becoming friend with him and So Young Pi has been a privilege. Looking back at the last decades of the past century gives a sense without undue nostalgia, I think, that those were wonderful years for Theoretical Physics, years that have witnessed the preeminence of gauge field theories, deep interactions with modern geometry and topology, the overwhelming revival of string theory and remarkably fruitful interactions between particle and condensed matter physics as well as cosmology. Roman was a main actor in these developments and to be at his side and benefit from his guidance and insights at that time was most fortunate. Owing to his leadership and immense scholarship, also because he is a great mentor, Roman has always been surrounded by many and has thus arXiv:2004.13191v1 [physics.hist-ph] 27 Apr 2020 generated a splendid network of friends and colleagues. Sometimes, with my own students, I reminisce about how it was in those days; I believe it is useful to keep a memory of the way some important ideas shaped up and were relayed. -
Particle - Mirror Particle Oscillations: CP-Violation and Baryon Asymmetry
Particle - Mirror Particle Oscillations: CP-violation and Baryon Asymmetry Zurab Berezhiani Università di L’Aquila and LNGS, Italy 0 CPT at ICTP, Triest, 2-5 July 2008 n − n oscillations etc ... - p. 1/42 Alice & Mirror World Lewis Carroll, "Through the Looking-Glass" ‘Now, if you’ll only attend, Kitty, and not talk so much, I’ll tell you all my ideas about Looking-glass House. There’s the room you can see through the glass – that’s just the same ● Carrol’s Alice... ● Mirror World as our drawing-room, only the things go the other way... the books are something like our ● Mirror Particles ● Interactions books, only the words go the wrong way: I know that, because I’ve held up one of our books to ● B & L violation ● BBN demands the glass, and then they hold up one in the other room. I can see all of it – all but the bit just ● Present Cosmology ● Visible vs. Dark matter behind the fireplace. I do so wish I could see that bit! I want so to know whether they’ve a fire ● B vs. D – Fine Tuning demonstration ● Unification in the winter: you never can tell, you know, unless our fire smokes, and then smoke comes up ● Neutrino Mixing ● See-Saw in that room too – but that may be only pretence, just to make it look as if they had a fire... ● Leptogenesis: diagrams ● Leptogenesis: formulas ‘How would you like to leave in the Looking-glass House, Kitty? I wander if they’d give you milk ● Epochs ● Neutron mixing in there? But perhaps Looking-glass milk isn’t good to drink? Now we come to the passage: ● Neutron mixing ● Oscillation it’s very like our passage as far as you can see, only you know it may be quite on beyond. -
Glossary of Terms Absorption Line a Dark Line at a Particular Wavelength Superimposed Upon a Bright, Continuous Spectrum
Glossary of terms absorption line A dark line at a particular wavelength superimposed upon a bright, continuous spectrum. Such a spectral line can be formed when electromag- netic radiation, while travelling on its way to an observer, meets a substance; if that substance can absorb energy at that particular wavelength then the observer sees an absorption line. Compare with emission line. accretion disk A disk of gas or dust orbiting a massive object such as a star, a stellar-mass black hole or an active galactic nucleus. An accretion disk plays an important role in the formation of a planetary system around a young star. An accretion disk around a supermassive black hole is thought to be the key mecha- nism powering an active galactic nucleus. active galactic nucleus (agn) A compact region at the center of a galaxy that emits vast amounts of electromagnetic radiation and fast-moving jets of particles; an agn can outshine the rest of the galaxy despite being hardly larger in volume than the Solar System. Various classes of agn exist, including quasars and Seyfert galaxies, but in each case the energy is believed to be generated as matter accretes onto a supermassive black hole. adaptive optics A technique used by large ground-based optical telescopes to remove the blurring affects caused by Earth’s atmosphere. Light from a guide star is used as a calibration source; a complicated system of software and hardware then deforms a small mirror to correct for atmospheric distortions. The mirror shape changes more quickly than the atmosphere itself fluctuates. -
Classical String Theory
PROSEMINAR IN THEORETICAL PHYSICS Classical String Theory ETH ZÜRICH APRIL 28, 2013 written by: DAVID REUTTER Tutor: DR.KEWANG JIN Abstract The following report is based on my talk about classical string theory given at April 15, 2013 in the course of the proseminar ’conformal field theory and string theory’. In this report a short historical and theoretical introduction to string theory is given. This is fol- lowed by a discussion of the point particle action, leading to the postulation of the Nambu-Goto and Polyakov action for the classical bosonic string. The equations of motion from these actions are derived, simplified and generally solved. Subsequently the Virasoro modes appearing in the solution are discussed and their algebra under the Poisson bracket is examined. 1 Contents 1 Introduction 3 2 The Relativistic String4 2.1 The Action of a Classical Point Particle..........................4 2.2 The General p-Brane Action................................6 2.3 The Nambu Goto Action..................................7 2.4 The Polyakov Action....................................9 2.5 Symmetries of the Action.................................. 11 3 Wave Equation and Solutions 13 3.1 Conformal Gauge...................................... 13 3.2 Equations of Motion and Boundary Terms......................... 14 3.3 Light Cone Coordinates................................... 15 3.4 General Solution and Oscillator Expansion......................... 16 3.5 The Virasoro Constraints.................................. 19 3.6 The Witt Algebra in Classical String Theory........................ 22 2 1 Introduction In 1969 the physicists Yoichiro Nambu, Holger Bech Nielsen and Leonard Susskind proposed a model for the strong interaction between quarks, in which the quarks were connected by one-dimensional strings holding them together. However, this model - known as string theory - did not really succeded in de- scribing the interaction. -
Mirror Matter: Astrophysical Implications
Mirror Matter: Astrophysical implications Zurab Berezhiani Summary Mirror Matter: Astrophysical implications Introduction: Dark Matter from a Parallel World Chapter I: Neutrino - mirror neutrino mixings Zurab Berezhiani Chapter II: neutron { mirror University of L'Aquila and LNGS neutron mixing Chapter IV: n − n0 and Neutron Stars Quarks-2021 , 22-24 June 2021 Contents Mirror Matter: Astrophysical implications Zurab Berezhiani Summary Introduction: Dark Matter from 1 Introduction: Dark Matter from a Parallel World a Parallel World Chapter I: Neutrino - mirror neutrino mixings 2 Chapter I: Neutrino - mirror neutrino mixings Chapter II: neutron { mirror neutron mixing Chapter IV: n − n0 and 3 Chapter II: neutron { mirror neutron mixing Neutron Stars 4 Chapter IV: n n0 and Neutron Stars − Mirror Matter: Astrophysical implications Zurab Berezhiani Summary Introduction: Dark Matter from a Parallel World Introduction Chapter I: Neutrino - mirror neutrino mixings Chapter II: neutron { mirror neutron mixing Chapter IV: n − n0 and Everything can be explained by the Standard Model ! Neutron Stars ... but there should be more than one Standard Models Bright & Dark Sides of our Universe Mirror Matter: Ω 0 05 observable matter: electron, proton, neutron ! Astrophysical B : implications ' ΩD 0:25 dark matter: WIMP? axion? sterile ν? ... Zurab Berezhiani ' ΩΛ 0:70 dark energy: Λ-term? Quintessence? .... Summary ' 3 Introduction: ΩR < 10− relativistic fraction: relic photons and neutrinos Dark Matter from a Parallel World Matter { dark energy coincidence: Ω Ω 0 45, (Ω = Ω + Ω ) Chapter I: M = Λ : M D B Neutrino - mirror 3 ' ρΛ Const., ρM a− ; why ρM /ρΛ 1 { just Today? neutrino mixings ∼ ∼ ∼ Chapter II: Antrophic explanation: if not Today, then Yesterday or Tomorrow. -
Lecture 4: Dark Matter in Galaxies
LectureLecture 4:4: DarkDark MatterMatter inin GalaxiesGalaxies OutlineOutline WhatWhat isis darkdark matter?matter? HowHow muchmuch darkdark mattermatter isis therethere inin thethe Universe?Universe? EvidenceEvidence ofof darkdark mattermatter ViableViable darkdark mattermatter candidatescandidates TheThe coldcold darkdark mattermatter (CDM)(CDM) modelmodel ProblemsProblems withwith CDMCDM onon galacticgalactic scalesscales AlternativesAlternatives toto darkdark mattermatter WhatWhat isis DarkDark Matter?Matter? Dark Matter Luminous Matter FirstFirst detectiondetection ofof darkdark mattermatter FritzFritz ZwickyZwicky (1933):(1933): DarkDark mattermatter inin thethe ComaComa ClusterCluster HowHow MuchMuch DarkDark MatterMatter isis ThereThere inin TheThe Universe?Universe? ΩΩ == ρρ // ρρ Μ Μ c ~2% RecentRecent measurements:measurements: (Luminous) Ω ∼ 0.25, Ω ∼ 0.75 ΩΜ ∼ 0.25, Ω Λ ∼ 0.75 ΩΩ ∼∼ 0.0050.005 Lum ~98% (Dark) HowHow DoDo WeWe KnowKnow ThatThat itit Exists?Exists? CosmologicalCosmological ParametersParameters ++ InventoryInventory ofof LuminousLuminous materialmaterial DynamicsDynamics ofof galaxiesgalaxies DynamicsDynamics andand gasgas propertiesproperties ofof galaxygalaxy clustersclusters GravitationalGravitational LensingLensing DynamicsDynamics ofof GalaxiesGalaxies II Galaxy ≈ Stars + Gas + Dust + Supermassive Black Hole + Dark Matter DynamicsDynamics ofof GalaxiesGalaxies IIII Visible galaxy Observed Vrot Expected R R Dark matter halo Visible galaxy DynamicsDynamics ofof GalaxyGalaxy ClustersClusters Balance -
Cosmological Reflection of Particle Symmetry
S S symmetry Review Cosmological Reflection of Particle Symmetry Maxim Khlopov 1,2 1 Laboratory of Astroparticle Physics and Cosmology 10, rue Alice Domon et Léonie Duquet, 75205 Paris Cedex 13, France; [email protected] 2 Center for Cosmopartcile Physics “Cosmion” and National Research Nuclear University “MEPHI” (Moscow State Engineering Physics Institute), Kashirskoe Shosse 31, Moscow 115409, Russia Academic Editor: Sergei D. Odintsov Received: 31 May 2016; Accepted: 10 August 2016; Published: 20 August 2016 Abstract: The standard model involves particle symmetry and the mechanism of its breaking. Modern cosmology is based on inflationary models with baryosynthesis and dark matter/energy, which involves physics beyond the standard model. Studies of the physical basis of modern cosmology combine direct searches for new physics at accelerators with its indirect non-accelerator probes, in which cosmological consequences of particle models play an important role. The cosmological reflection of particle symmetry and the mechanisms of its breaking are the subject of the present review. Keywords: elementary particles; dark matter; early universe; symmetry breaking 1. Introduction The laws of known particle interactions and transformations are based on the gauge symmetry-extension of the gauge principle of quantum electrodynamics to strong and weak interactions. Starting from isotopic invariance of nuclear forces, treating proton and neutron as different states of one particle-nucleon; the development of this approach led to the successful -
Pos(CORFU2016)050
F(750), We Miss You as a Bound State of 6 Top and 6 Antitop Quarks, Multiple Point Principle PoS(CORFU2016)050 Holger F. Bech Nielsen∗ y Niels Bohr Institute, Blegdamvej 15-21, DK 2100 Copenhagen Ø, Denmark D.L. Bennett Brooks Institute, Copenhagen, Denmark C.R. Das z BLTP, JINR, Dubna, Moscow, Russia C.D. Froggatt § Glasgow University, Glasgow, UK L.V. Laperashvili { ITEP, National Research Center “Kurchatov Institute”, Moscow, Russia We review our speculation, that in the pure Standard Model the exchange of Higgses, including also the ones “eaten by W ± and Z”, and of gluons together make a bound state of 6 top plus 6 anti top quarks bind so strongly that its mass gets down to about 1/3 of the mass of the collective mass 12 mt of the 12 constituent quarks. The true importance of this speculated bound state is that it makes it possible to uphold, even inside the Standard Mode, our proposal for what is really a new law of nature saying that there are several phases of empty space, vacua, all having very small energy densities (of the order of the present energy density in the universe). The reason suggested for believing in this new law called the “Multiple (Criticality) Point Principle” is, that estimating the mass of the speculated bound state using the “Multiple Point Principle” leads to two consistent mass-values; and they even agree with a crude bag-model like estimate of the mass of this bound state. Very unfortunately the statistical fluctuation so popular last year when interpreted as the digamma resonance F(750) turned out not to be a real resonance, because our estimated bound state mass is just around the mass of 750 GeV.