Structure of Matter
Total Page:16
File Type:pdf, Size:1020Kb
Load more
Recommended publications
-
Searches for Electroweak Production of Supersymmetric Gauginos and Sleptons and R-Parity Violating and Long-Lived Signatures with the ATLAS Detector
Searches for electroweak production of supersymmetric gauginos and sleptons and R-parity violating and long-lived signatures with the ATLAS detector Ruo yu Shang University of Illinois at Urbana-Champaign (for the ATLAS collaboration) Supersymmetry (SUSY) • Standard model does not answer: What is dark matter? Why is the mass of Higgs not at Planck scale? • SUSY states the existence of the super partners whose spin differing by 1/2. • A solution to cancel the quantum corrections and restore the Higgs mass. • Also provides a potential candidate to dark matter with a stable WIMP! 2 Search for SUSY at LHC squark gluino 1. Gluino, stop, higgsino are the most important ones to the problem of Higgs mass. 2. Standard search for gluino/squark (top- right plots) usually includes • large jet multiplicity • missing energy ɆT carried away by lightest SUSY particle (LSP) • See next talk by Dr. Vakhtang TSISKARIDZE. 3. Dozens of analyses have extensively excluded gluino mass up to ~2 TeV. Still no sign of SUSY. 4. What are we missing? 3 This talk • Alternative searches to probe supersymmetry. 1. Search for electroweak SUSY 2. Search for R-parity violating SUSY. 3. Search for long-lived particles. 4 Search for electroweak SUSY Look for strong interaction 1. Perhaps gluino mass is beyond LHC energy scale. gluino ↓ 2. Let’s try to find gauginos! multi-jets 3. For electroweak productions we look for Look for electroweak interaction • leptons (e/μ/τ) from chargino/neutralino decay. EW gaugino • ɆT carried away by LSP. ↓ multi-leptons 5 https://cds.cern.ch/record/2267406 Neutralino/chargino via WZ decay 2� 3� 2� SR ɆT [GeV] • Models assume gauginos decay to W/Z + LSP. -
Wimps and Machos ENCYCLOPEDIA of ASTRONOMY and ASTROPHYSICS
WIMPs and MACHOs ENCYCLOPEDIA OF ASTRONOMY AND ASTROPHYSICS WIMPs and MACHOs objects that could be the dark matter and still escape detection. For example, if the Galactic halo were filled –3 . WIMP is an acronym for weakly interacting massive par- with Jupiter mass objects (10 Mo) they would not have ticle and MACHO is an acronym for massive (astrophys- been detected by emission or absorption of light. Brown . ical) compact halo object. WIMPs and MACHOs are two dwarf stars with masses below 0.08Mo or the black hole of the most popular DARK MATTER candidates. They repre- remnants of an early generation of stars would be simi- sent two very different but reasonable possibilities of larly invisible. Thus these objects are examples of what the dominant component of the universe may be. MACHOs. Other examples of this class of dark matter It is well established that somewhere between 90% candidates include primordial black holes created during and 99% of the material in the universe is in some as yet the big bang, neutron stars, white dwarf stars and vari- undiscovered form. This material is the gravitational ous exotic stable configurations of quantum fields, such glue that holds together galaxies and clusters of galaxies as non-topological solitons. and plays an important role in the history and fate of the An important difference between WIMPs and universe. Yet this material has not been directly detected. MACHOs is that WIMPs are non-baryonic and Since extensive searches have been done, this means that MACHOS are typically (but not always) formed from this mysterious material must not emit or absorb appre- baryonic material. -
The Nobel Prize in Physics 1999
The Nobel Prize in Physics 1999 The last Nobel Prize of the Millenium in Physics has been awarded jointly to Professor Gerardus ’t Hooft of the University of Utrecht in Holland and his thesis advisor Professor Emeritus Martinus J.G. Veltman of Holland. According to the Academy’s citation, the Nobel Prize has been awarded for ’elucidating the quantum structure of electroweak interaction in Physics’. It further goes on to say that they have placed particle physics theory on a firmer mathematical foundation. In this short note, we will try to understand both these aspects of the award. The work for which they have been awarded the Nobel Prize was done in 1971. However, the precise predictions of properties of particles that were made possible as a result of their work, were tested to a very high degree of accuracy only in this last decade. To understand the full significance of this Nobel Prize, we will have to summarise briefly the developement of our current theoretical framework about the basic constituents of matter and the forces which hold them together. In fact the path can be partially traced in a chain of Nobel prizes starting from one in 1965 to S. Tomonaga, J. Schwinger and R. Feynman, to the one to S.L. Glashow, A. Salam and S. Weinberg in 1979, and then to C. Rubia and Simon van der Meer in 1984 ending with the current one. In the article on ‘Search for a final theory of matter’ in this issue, Prof. Ashoke Sen has described the ‘Standard Model (SM)’ of particle physics, wherein he has listed all the elementary particles according to the SM. -
MASTER THESIS Linking the B-Physics Anomalies and Muon G
MSc PHYSICS AND ASTRONOMY GRAVITATION, ASTRO-, AND PARTICLE PHYSICS MASTER THESIS Linking the B-physics Anomalies and Muon g − 2 A Phenomenological Study Beyond the Standard Model By Anders Rehult 12623881 February - October 2020 60 EC Supervisor/Examiner: Second Examiner: prof. dr. Robert Fleischer prof. dr. Piet Mulders i Abstract The search for physics beyond the Standard Model is guided by anomalies: discrepancies between the theoretical predictions and experimental measurements of physical quantities. Hints of new physics are found in the recently observed B-physics anomalies and the long-standing anomalous magnetic dipole moment of the muon, muon g − 2. The former include a group of anomalous measurements related to the quark-level transition b ! s. We investigate what features are required of a theory to explain these b ! s anomalies simultaneously with muon g − 2. We then consider three kinds of models that might explain the anomalies: models with leptoquarks, hypothetical particles that couple leptons to quarks; Z0 models, which contain an additional fundamental force and a corresponding force carrier; and supersymmetric scenarios that postulate a symmetry that gives rise to a partner for each SM particle. We identify a leptoquark model that carries the necessary features to explain both kinds of anomalies. Within this model, we study the behaviour of 0 muon g − 2 and the anomalous branching ratio of Bs mesons, bound states of b and s quarks, into muons. 0 ¯0 0 ¯0 The Bs meson can spontaneously oscillate into its antiparticle Bs , a phenomenon known as Bs −Bs mixing. We calculate the effects of this mixing on the anomalous branching ratio. -
Week 3: Thermal History of the Universe
Week 3: Thermal History of the Universe Cosmology, Ay127, Spring 2008 April 21, 2008 1 Brief Overview Before moving on, let’s review some of the high points in the history of the Universe: T 10−4 eV, t 1010 yr: today; baryons and the CMB are entirely decoupled, stars and • ∼ ∼ galaxies have been around a long time, and clusters of galaxies (gravitationally bound systems of 1000s of galaxies) are becoming common. ∼ T 10−3 eV, t 109 yr; the first stars and (small) galaxies begin to form. • ∼ ∼ T 10−1−2 eV, t millions of years: baryon drag ends; at earlier times, the baryons are still • ∼ ∼ coupled to the CMB photons, and so perturbations in the baryon cannot grow; before this time, the gas distribution in the Universe remains smooth. T eV, t 400, 000 yr: electrons and protons combine to form hydrogen atoms, and CMB • ∼ ∼ photons decouple; at earlier times, photons are tightly coupled to the baryon fluid through rapid Thomson scattering from free electrons. T 3 eV, t 10−(4−5) yrs: matter-radiation equality; at earlier times, the energy den- • ∼ ∼ sity of the Universe is dominated by radiation. Nothing really spectacular happens at this time, although perturbations in the dark-matter density can begin to grow, providing seed gravitational-potential wells for what will later become the dark-matter halos that house galaxies and clusters of galaxies. T keV, t 105 sec; photons fall out of chemical equilibrium. At earlier times, interac- • ∼ ∼ tions that can change the photon number occur rapidly compared with the expansion rate; afterwards, these reactions freeze out and CMB photons are neither created nor destroyed. -
Electro-Weak Interactions
Electro-weak interactions Marcello Fanti Physics Dept. | University of Milan M. Fanti (Physics Dep., UniMi) Fundamental Interactions 1 / 36 The ElectroWeak model M. Fanti (Physics Dep., UniMi) Fundamental Interactions 2 / 36 Electromagnetic vs weak interaction Electromagnetic interactions mediated by a photon, treat left/right fermions in the same way g M = [¯u (eγµ)u ] − µν [¯u (eγν)u ] 3 1 q2 4 2 1 − γ5 Weak charged interactions only apply to left-handed component: = L 2 Fermi theory (effective low-energy theory): GF µ 5 ν 5 M = p u¯3γ (1 − γ )u1 gµν u¯4γ (1 − γ )u2 2 Complete theory with a vector boson W mediator: g 1 − γ5 g g 1 − γ5 p µ µν p ν M = u¯3 γ u1 − 2 2 u¯4 γ u2 2 2 q − MW 2 2 2 g µ 5 ν 5 −−−! u¯3γ (1 − γ )u1 gµν u¯4γ (1 − γ )u2 2 2 low q 8 MW p 2 2 g −5 −2 ) GF = | and from weak decays GF = (1:1663787 ± 0:0000006) · 10 GeV 8 MW M. Fanti (Physics Dep., UniMi) Fundamental Interactions 3 / 36 Experimental facts e e Electromagnetic interactions γ Conserves charge along fermion lines ¡ Perfectly left/right symmetric e e Long-range interaction electromagnetic µ ) neutral mass-less mediator field A (the photon, γ) currents eL νL Weak charged current interactions Produces charge variation in the fermions, ∆Q = ±1 W ± Acts only on left-handed component, !! ¡ L u Short-range interaction L dL ) charged massive mediator field (W ±)µ weak charged − − − currents E.g. -
ELECTROWEAK PHYSICS Theory for the Experimentalist
ELECTROWEAK PHYSICS Theory for the experimentalist Chris Hays Oxford University CONTENTS Introduction vii 1 The geometry of forces 1 1.1 The fiber bundle of the universe 2 1.2 Spacetime metric 3 1.3 Connections 5 1.4 Curvature 6 1.5 Principle of least action 7 1.6 Conservation laws 9 2 Path integrals and fields 11 2.1 Non-relativistic path integral 12 2.2 Perturbation theory 13 2.2.1 Green’s functions 14 2.3 Path integral of a scalar field 15 2.3.1 Free-field transition amplitude 16 2.3.2 Interacting-field transition amplitude 17 2.4 Path integral of a fermion field 18 2.5 Path integral of a gauge field 19 2.5.1 Free-field generating functional 21 3 The Higgs mechanism 23 iii iv CONTENTS 3.1 Self-interacting scalar field theory 23 3.1.1 Real scalar field 23 3.1.2 Complex scalar field 24 3.2 Gauged scalar field theory 25 3.2.1 U(1)-charged scalar field 25 3.2.2 SU(2)-charged scalar field 26 3.2.3 Propagators after symmetry breaking 27 4 The Electroweak theory 29 4.1 The Electroweak Lagrangian 29 4.2 Electroweak symmetry breaking 30 4.2.1 Scalar field Lagrangian 31 4.2.2 Fermion field Lagrangian 33 4.3 Electroweak propagators 34 5 Cross sections and Feynman diagrams 37 5.1 Scattering matrix 37 5.2 Cross sections and lifetimes 38 5.3 Feynman rules 40 6 Scalar renormalization 47 6.1 Renormalized Lagrangian 47 6.2 Regularization 49 6.2.1 Propagator loop corrections 49 6.2.2 Vertex loop correction 50 6.3 The renormalization group 51 7 QED renormalization 55 7.1 QED divergences 55 7.2 Fermion self energy 56 7.3 Vacuum polarization 57 7.4 Vertex correction 61 -
Supersymmetry in the Shadow of Photini
Photini in the UV Photini in the IR Photini at the LHC Supersymmetry in the shadow of photini Ken Van Tilburg August 24, 2012 In collaboration with: Masha Baryakhtar (Stanford), Nathaniel Craig (Rutgers, IAS) Reference: arXiv:1206.0751; JHEP 1207 (2012) 164 Arvanitaki et al: arXiv:0909:5440; Phys.Rev.D81 (2010) 075018 1/6 Photini in the UV Photini in the IR Photini at the LHC Table of contents 1 Photini in the UV 2 Photini in the IR 3 Photini at the LHC 2/6 Photini in the UV Photini in the IR Photini at the LHC Photini in the UV Main features of string theory: 1 supersymmetry assume broken at low energy to solve hierarchy problem 2 extra dimensions (6) assume small size generically complex compactification manifold to get SM very simple manifold: 6-torus ! six 1- and 5-cycles, fifteen 2- and 4-cycles, twenty 3-cycles IIB string theory: 4-form gauge field integrated over 3-cycle i R ! 4D vector gauge field without charged matter Aµ = C4 Σi string theory ! SUSY SM many extra \photon" superfields without any charged matter can in principle mix with U(1) hypercharge and among each other 3/6 Photini in the UV Photini in the IR Photini at the LHC Photini in the IR in SUSY limit, no observable effect: Z 2 L ⊃ d θ WaWa + WbWb − 2WaWb shift away mixing: W ! W − W and g ! p ga b b a a 1−2 physical effects from SUSY breaking, when gauginos get mass y µ δL ⊃ zijλi iσ @µλj − mijλi λj expect sizeable number of photini to be lighter than the bino bino-photino + interphotini cascade via emissions of h; Z; γ 4/6 gluino-bino model gluino-squark-bino model drastically weakened hadronic search limits: slightly enhanced leptonic search sensitivity: Photini in the UV Photini in the IR Photini at the LHC Photini at the LHC reduction of missing ET 1.0 bino 150 GeV L . -
New Heavy Resonances: from the Electroweak to the Planck Scale
New heavy resonances : from the electroweak to the planck scale Florian Lyonnet To cite this version: Florian Lyonnet. New heavy resonances : from the electroweak to the planck scale. High Energy Physics - Phenomenology [hep-ph]. Université de Grenoble, 2014. English. NNT : 2014GRENY035. tel-01110759v2 HAL Id: tel-01110759 https://tel.archives-ouvertes.fr/tel-01110759v2 Submitted on 10 Apr 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. THÈSE Pour obtenirle grade de DOCTEUR DE L’UNIVERSITÉ DE GRENOBLE Spécialité:Physique Subatomiqueet Astroparticules Arrêtéministériel:7août2006 Présentéepar FlorianLyonnet ThèsedirigéeparIngoSchienbein préparéeau sein Laboratoirede Physique Subatomiqueet de Cosmolo- gie et de Ecoledoctoralede physique de Grenoble New heavy resonances: from the Electroweak to thePlanck scale ThèsesoutenuepubliquementOH VHSWHPEUH , devant le jurycomposéde : Mr. Aldo,Deandrea Prof., UniversitéClaudeBernardLyon 1, Rapporteur Mr. Jean-Loïc,Kneur DR,LaboratoireCharlesCoulombMontpellier,Rapporteur Mr. Roberto Bonciani Dr., UniversitàdegliStudidi Roma”LaSapienza”,Examinateur Mr. MichaelKlasen Prof., UniversitätMünster,Examinateur Mr. FrançoisMontanet Prof.,UniversitéJosephFourierde Grenoble,3UpVLGHQW Mr. JeanOrloff Prof., UniversitéBlaisePascal de Clermont-Ferrand,Examinateur Mr. IngoSchienbein MCF., UniversitéJosephFourier, Directeurde thèse ACKNOWLEDMENGTS My years at the LPSC have been exciting, intense, and I would like to express my sincere gratitude to all the people that contributed to it on the professional as well as personal level. -
The Charm of Theoretical Physics (1958– 1993)?
Eur. Phys. J. H 42, 611{661 (2017) DOI: 10.1140/epjh/e2017-80040-9 THE EUROPEAN PHYSICAL JOURNAL H Oral history interview The Charm of Theoretical Physics (1958{ 1993)? Luciano Maiani1 and Luisa Bonolis2,a 1 Dipartimento di Fisica and INFN, Piazzale A. Moro 5, 00185 Rome, Italy 2 Max Planck Institute for the History of Science, Boltzmannstraße 22, 14195 Berlin, Germany Received 10 July 2017 / Received in final form 7 August 2017 Published online 4 December 2017 c The Author(s) 2017. This article is published with open access at Springerlink.com Abstract. Personal recollections on theoretical particle physics in the years when the Standard Theory was formed. In the background, the remarkable development of Italian theoretical physics in the second part of the last century, with great personalities like Bruno Touschek, Raoul Gatto, Nicola Cabibbo and their schools. 1 Apprenticeship L. B. How did your interest in physics arise? You enrolled in the late 1950s, when the period of post-war reconstruction of physics in Europe was coming to an end, and Italy was entering into a phase of great expansion. Those were very exciting years. It was the beginning of the space era. L. M. The beginning of the space era certainly had a strong influence on many people, absolutely. The landing on the moon in 1969 was for sure unforgettable, but at that time I was already working in Physics and about to get married. My interest in physics started well before. The real beginning was around 1955. Most important for me was astronomy. It is not surprising that astronomy marked for many people the beginning of their interest in science. -
Abdus Salam United Nations Educational, Scientific and Cultural Organization International XAO100669 Centre •I,'
the IC/2000/182 abdus salam united nations educational, scientific and cultural organization international XAO100669 centre •i,' international atomic energy agency for theoretical physics " F ^9 -- •.'— -> J AXINO PRODUCTION IN e+e" AND yy COLLISIONS Hoang Ngoc Long and Dang Van Soa 32/ 17 Available at: http://www.ictp.trieste.it/~pub-off IC/2000/182 United Nations Educational Scientific and Cultural Organization and International Atomic Energy Agency THE ABDUS SALAM INTERNATIONAL CENTRE FOR THEORETICAL PHYSICS AXINO PRODUCTION IN e+e" AND 77 COLLISIONS Hoang Ngoc Long Institute of Physics, NCST, P.O. Box 429, Bo Ho, Hanoi 10000, Vietnam1 and The Abdus Salam International Centre for Theoretical Physics, Trieste, Italy and Dang Van Soa Department of Physics, Hanoi University of Mining and Geology, Dong Ngac, Tu Liem, Hanoi, Vietnam1 and The Abdus Salam International Centre for Theoretical Physics, Trieste, Italy. Abstract Production of axinos and photinos in e+e~ and 77 collisions is calculated and estimated. It is shown that there is an upper limit of the cross section for the process e~e+ —> ayc dependent only on the breaking scale. For the process 77 —> aac, there is a special direction in which axinos are mainly produced. Behaviour of cross section for this process is also analysed. Based on the result a new constraint for F/N is derived: j^ > 1014 GeV. MIRAMARE - TRIESTE December 2000 1 Permanent address. Axinos - supersymmetric partners of axions [1-3] are predicted in low-energy supersym- metry and the Peccei-Quinn (PQ) solution. The axino is an electrically and color neutral particle with mass highly dependent of the models [4-6]. -
I . .- SLAC-PUB-4497 - May 1988 T/E/AS
I . .- SLAC-PUB-4497 - May 1988 T/E/AS BOLOMETRIC DETECTION OF COLD DARK MATTER CANDIDATES: Some Material Considerations* A. K. DRUKIER Applied Research Corporation 8201 Corporate Drive, Suite 920 Landover, MD 20785 and Physics Department University of Maryland College Park, MD 20742 and KATHERINE FREESE’ Department of Astronomy Ufliversity of California Berkeley, CA 94720 -. - and JOSHUA FRIEMAN Stanford Linear Accelerator Center Stanford University, Stanford, California 94309 Submitted to Journal of Applied Physics - * Work supported by the Department of Energy, contract DE-AC03-76SF00515. + Present address: Dept. of Physics, Massachussetts Institute of Technology, Cambridge, MA 02139 ABSTRACT We discuss the use of crystal bolometers to search for weakly interacting cold dark matter particles in the galactic halo. For particles with spin dependent nuclear interactions, such as photinos, Majorana neutrinos and higgsinos, we show that compounds of boron, lithium, or fluorine are optimal detector components. We give careful estimates of expected cross-sections and event rates and discuss optimal -. - detector granularities. 2 - 1. Introduction The rotation curves of spiral galaxies are flat out to large radii, indicating that galactic halos extend out far beyond the visible matter.’ If this dark matter is non- baryonic, as suggested by a variety of arguments: it may consist of one of several exotic candidates. Weakly interacting massive particles (WIMPS) are candidates in the GeV mass range which interact with ordinary matter with cross sections O( 10-38) cm2. WIMPS can be divided into two classes: (I) those with coherent interactions on matter, i.e., cross-sections o( N2, where N is approximately the atomic number of the scattering nucleus.