Review of Lepton Universality Tests in B Decays
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The Five Common Particles
The Five Common Particles The world around you consists of only three particles: protons, neutrons, and electrons. Protons and neutrons form the nuclei of atoms, and electrons glue everything together and create chemicals and materials. Along with the photon and the neutrino, these particles are essentially the only ones that exist in our solar system, because all the other subatomic particles have half-lives of typically 10-9 second or less, and vanish almost the instant they are created by nuclear reactions in the Sun, etc. Particles interact via the four fundamental forces of nature. Some basic properties of these forces are summarized below. (Other aspects of the fundamental forces are also discussed in the Summary of Particle Physics document on this web site.) Force Range Common Particles It Affects Conserved Quantity gravity infinite neutron, proton, electron, neutrino, photon mass-energy electromagnetic infinite proton, electron, photon charge -14 strong nuclear force ≈ 10 m neutron, proton baryon number -15 weak nuclear force ≈ 10 m neutron, proton, electron, neutrino lepton number Every particle in nature has specific values of all four of the conserved quantities associated with each force. The values for the five common particles are: Particle Rest Mass1 Charge2 Baryon # Lepton # proton 938.3 MeV/c2 +1 e +1 0 neutron 939.6 MeV/c2 0 +1 0 electron 0.511 MeV/c2 -1 e 0 +1 neutrino ≈ 1 eV/c2 0 0 +1 photon 0 eV/c2 0 0 0 1) MeV = mega-electron-volt = 106 eV. It is customary in particle physics to measure the mass of a particle in terms of how much energy it would represent if it were converted via E = mc2. -
Decays of the Tau Lepton*
SLAC - 292 UC - 34D (E) DECAYS OF THE TAU LEPTON* Patricia R. Burchat Stanford Linear Accelerator Center Stanford University Stanford, California 94305 February 1986 Prepared for the Department of Energy under contract number DE-AC03-76SF00515 Printed in the United States of America. Available from the National Techni- cal Information Service, U.S. Department of Commerce, 5285 Port Royal Road, Springfield, Virginia 22161. Price: Printed Copy A07, Microfiche AOl. JC Ph.D. Dissertation. Abstract Previous measurements of the branching fractions of the tau lepton result in a discrepancy between the inclusive branching fraction and the sum of the exclusive branching fractions to final states containing one charged particle. The sum of the exclusive branching fractions is significantly smaller than the inclusive branching fraction. In this analysis, the branching fractions for all the major decay modes are measured simultaneously with the sum of the branching fractions constrained to be one. The branching fractions are measured using an unbiased sample of tau decays, with little background, selected from 207 pb-l of data accumulated with the Mark II detector at the PEP e+e- storage ring. The sample is selected using the decay products of one member of the r+~- pair produced in e+e- annihilation to identify the event and then including the opposite member of the pair in the sample. The sample is divided into subgroups according to charged and neutral particle multiplicity, and charged particle identification. The branching fractions are simultaneously measured using an unfold technique and a maximum likelihood fit. The results of this analysis indicate that the discrepancy found in previous experiments is possibly due to two sources. -
Lepton Flavor and Number Conservation, and Physics Beyond the Standard Model
Lepton Flavor and Number Conservation, and Physics Beyond the Standard Model Andr´ede Gouv^ea1 and Petr Vogel2 1 Department of Physics and Astronomy, Northwestern University, Evanston, Illinois, 60208, USA 2 Kellogg Radiation Laboratory, Caltech, Pasadena, California, 91125, USA April 1, 2013 Abstract The physics responsible for neutrino masses and lepton mixing remains unknown. More ex- perimental data are needed to constrain and guide possible generalizations of the standard model of particle physics, and reveal the mechanism behind nonzero neutrino masses. Here, the physics associated with searches for the violation of lepton-flavor conservation in charged-lepton processes and the violation of lepton-number conservation in nuclear physics processes is summarized. In the first part, several aspects of charged-lepton flavor violation are discussed, especially its sensitivity to new particles and interactions beyond the standard model of particle physics. The discussion concentrates mostly on rare processes involving muons and electrons. In the second part, the sta- tus of the conservation of total lepton number is discussed. The discussion here concentrates on current and future probes of this apparent law of Nature via searches for neutrinoless double beta decay, which is also the most sensitive probe of the potential Majorana nature of neutrinos. arXiv:1303.4097v2 [hep-ph] 29 Mar 2013 1 1 Introduction In the absence of interactions that lead to nonzero neutrino masses, the Standard Model Lagrangian is invariant under global U(1)e × U(1)µ × U(1)τ rotations of the lepton fields. In other words, if neutrinos are massless, individual lepton-flavor numbers { electron-number, muon-number, and tau-number { are expected to be conserved. -
Neutrino Opacity I. Neutrino-Lepton Scattering*
PHYSICAL REVIEW VOLUME 136, NUMBER 4B 23 NOVEMBER 1964 Neutrino Opacity I. Neutrino-Lepton Scattering* JOHN N. BAHCALL California Institute of Technology, Pasadena, California (Received 24 June 1964) The contribution of neutrino-lepton scattering to the total neutrino opacity of matter is investigated; it is found that, contrary to previous beliefs, neutrino scattering dominates the neutrino opacity for many astro physically important conditions. The rates for neutrino-electron scattering and antineutrino-electron scatter ing are given for a variety of conditions, including both degenerate and nondegenerate gases; the rates for some related reactions are also presented. Formulas are given for the mean scattering angle and the mean energy loss in neutrino and antineutrino scattering. Applications are made to the following problems: (a) the detection of solar neutrinos; (b) the escape of neutrinos from stars; (c) neutrino scattering in cosmology; and (d) energy deposition in supernova explosions. I. INTRODUCTION only been discussed for the special situation of electrons 13 14 XPERIMENTS1·2 designed to detect solar neu initially at rest. · E trinos will soon provide crucial tests of the theory In this paper, we investigate the contribution of of stellar energy generation. Other neutrino experiments neutrino-lepton scattering to the total neutrino opacity have been suggested as a test3 of a possible mechanism of matter and show, contrary to previous beliefs, that for producing the high-energy electrons that are inferred neutrino-lepton scattering dominates the neutrino to exist in strong radio sources and as a means4 for opacity for many astrophysically important conditions. studying the high-energy neutrinos emitted in the decay Here, neutrino opacity is defined, analogously to photon of cosmic-ray secondaries. -
Snowmass 2021 Letter of Interest: Hadron Spectroscopy at Belle II
Snowmass 2021 Letter of Interest: Hadron Spectroscopy at Belle II on behalf of the U.S. Belle II Collaboration D. M. Asner1, Sw. Banerjee2, J. V. Bennett3, G. Bonvicini4, R. A. Briere5, T. E. Browder6, D. N. Brown2, C. Chen7, D. Cinabro4, J. Cochran7, L. M. Cremaldi3, A. Di Canto1, K. Flood6, B. G. Fulsom8, R. Godang9, W. W. Jacobs10, D. E. Jaffe1, K. Kinoshita11, R. Kroeger3, R. Kulasiri12, P. J. Laycock1, K. A. Nishimura6, T. K. Pedlar13, L. E. Piilonen14, S. Prell7, C. Rosenfeld15, D. A. Sanders3, V. Savinov16, A. J. Schwartz11, J. Strube8, D. J. Summers3, S. E. Vahsen6, G. S. Varner6, A. Vossen17, L. Wood8, and J. Yelton18 1Brookhaven National Laboratory, Upton, New York 11973 2University of Louisville, Louisville, Kentucky 40292 3University of Mississippi, University, Mississippi 38677 4Wayne State University, Detroit, Michigan 48202 5Carnegie Mellon University, Pittsburgh, Pennsylvania 15213 6University of Hawaii, Honolulu, Hawaii 96822 7Iowa State University, Ames, Iowa 50011 8Pacific Northwest National Laboratory, Richland, Washington 99352 9University of South Alabama, Mobile, Alabama 36688 10Indiana University, Bloomington, Indiana 47408 11University of Cincinnati, Cincinnati, Ohio 45221 12Kennesaw State University, Kennesaw, Georgia 30144 13Luther College, Decorah, Iowa 52101 14Virginia Polytechnic Institute and State University, Blacksburg, Virginia 24061 15University of South Carolina, Columbia, South Carolina 29208 16University of Pittsburgh, Pittsburgh, Pennsylvania 15260 17Duke University, Durham, North Carolina 27708 18University of Florida, Gainesville, Florida 32611 Corresponding Author: B. G. Fulsom (Pacific Northwest National Laboratory), [email protected] Thematic Area(s): (RF07) Hadron Spectroscopy 1 Abstract: The Belle II experiment at the SuperKEKB energy-asymmetric e+e− collider is a substantial upgrade of the B factory facility at KEK in Tsukuba, Japan. -
1 Drawing Feynman Diagrams
1 Drawing Feynman Diagrams 1. A fermion (quark, lepton, neutrino) is drawn by a straight line with an arrow pointing to the left: f f 2. An antifermion is drawn by a straight line with an arrow pointing to the right: f f 3. A photon or W ±, Z0 boson is drawn by a wavy line: γ W ±;Z0 4. A gluon is drawn by a curled line: g 5. The emission of a photon from a lepton or a quark doesn’t change the fermion: γ l; q l; q But a photon cannot be emitted from a neutrino: γ ν ν 6. The emission of a W ± from a fermion changes the flavour of the fermion in the following way: − − − 2 Q = −1 e µ τ u c t Q = + 3 1 Q = 0 νe νµ ντ d s b Q = − 3 But for quarks, we have an additional mixing between families: u c t d s b This means that when emitting a W ±, an u quark for example will mostly change into a d quark, but it has a small chance to change into a s quark instead, and an even smaller chance to change into a b quark. Similarly, a c will mostly change into a s quark, but has small chances of changing into an u or b. Note that there is no horizontal mixing, i.e. an u never changes into a c quark! In practice, we will limit ourselves to the light quarks (u; d; s): 1 DRAWING FEYNMAN DIAGRAMS 2 u d s Some examples for diagrams emitting a W ±: W − W + e− νe u d And using quark mixing: W + u s To know the sign of the W -boson, we use charge conservation: the sum of the charges at the left hand side must equal the sum of the charges at the right hand side. -
Phenomenology of Gev-Scale Heavy Neutral Leptons Arxiv:1805.08567
Prepared for submission to JHEP INR-TH-2018-014 Phenomenology of GeV-scale Heavy Neutral Leptons Kyrylo Bondarenko,1 Alexey Boyarsky,1 Dmitry Gorbunov,2;3 Oleg Ruchayskiy4 1Intituut-Lorentz, Leiden University, Niels Bohrweg 2, 2333 CA Leiden, The Netherlands 2Institute for Nuclear Research of the Russian Academy of Sciences, Moscow 117312, Russia 3Moscow Institute of Physics and Technology, Dolgoprudny 141700, Russia 4Discovery Center, Niels Bohr Institute, Copenhagen University, Blegdamsvej 17, DK- 2100 Copenhagen, Denmark E-mail: [email protected], [email protected], [email protected], [email protected] Abstract: We review and revise phenomenology of the GeV-scale heavy neutral leptons (HNLs). We extend the previous analyses by including more channels of HNLs production and decay and provide with more refined treatment, including QCD corrections for the HNLs of masses (1) GeV. We summarize the relevance O of individual production and decay channels for different masses, resolving a few discrepancies in the literature. Our final results are directly suitable for sensitivity studies of particle physics experiments (ranging from proton beam-dump to the LHC) aiming at searches for heavy neutral leptons. arXiv:1805.08567v3 [hep-ph] 9 Nov 2018 ArXiv ePrint: 1805.08567 Contents 1 Introduction: heavy neutral leptons1 1.1 General introduction to heavy neutral leptons2 2 HNL production in proton fixed target experiments3 2.1 Production from hadrons3 2.1.1 Production from light unflavored and strange mesons5 2.1.2 -
Production of the Doubly Charged Higgs Boson in Association with the SM Gauge Bosons And/Or Other HTM Scalars at Hadron Colliders
S S symmetry Article Production of the Doubly Charged Higgs Boson in Association with the SM Gauge Bosons and/or Other HTM Scalars at Hadron Colliders Bartosz Dziewit 1,* , Magdalena Kordiaczy ´nska 1 and Tripurari Srivastava 2 1 Institute of Physics, University of Silesia, 40-007 Katowice, Poland; [email protected] 2 Department of Physics, DIT University Dehradun, Uttarakhand 248009, India; [email protected] * Correspondence: [email protected] Abstract: We investigate an extension of the Standard Model with one additional triplet of scalar bosons. Altogether, the model contains four Higgs bosons. We analyze the associated production of the doubly charged scalar with the Standard Model gauge bosons and the remaining Higgs bosons of the model, which are: the light (SM) and heavy neutral scalars and a singly charged scalar. We estimate, in the context of the present (HL–LHC) and future (FCC–hh) hadron colliders, the most promising processes in which a single produced doubly charged Higgs boson is involved. Keywords: theoretical physics; particle physics; Standard Model; Higgs triplets; doubly charged Higgs bosons; hadron colliders Citation: Dziewit, B.; Kordiaczy´nska, M.; Srivastava, T. Production of the Doubly Charged Higgs Boson in 1. Introduction Association with the SM Gauge Bosons and/or Other HTM Scalars at Experimental evidence of the Higgs boson’s existence, found at the Large Hadron Hadron Colliders. Symmetry 2021, 13, Collider (LHC) [1,2], was a quantum leap in particle physics history. Nevertheless, ques- 1240. https://doi.org/10.3390/ tions related to the minimal Higgs sector are still open. From this point of view, extensions sym13071240 of the Standard Model can be realized in two ways: directly, by introducing additional multiplets, or indirectly, by extending the gauge group (e.g., left right symmetric mod- Academic Editors: Zoltán Trócsányi, els [3–8]). -
Detectors for Extreme Luminosity: Belle II
Nuclear Inst. and Methods in Physics Research, A 907 (2018) 46–59 Contents lists available at ScienceDirect Nuclear Inst. and Methods in Physics Research, A journal homepage: www.elsevier.com/locate/nima Detectors for extreme luminosity: Belle II I. Adachi a,b , T.E. Browder c, P. Kriºan d,e, *, S. Tanaka a,b , Y. Ushiroda a,b,f , (on behalf of the Belle II Collaboration) a High Energy Accelerator Research Organization (KEK), Tsukuba, Japan b SOKENDAI (The Graduate University for Advanced Studies), Hayama 240-0193, Japan c University of Hawaii, Honolulu, HI, United States d Faculty of Mathematics and Physics, University of Ljubljana, Slovenia e Joºef Stefan Institute, Ljubljana, Slovenia f Department of Physics, Graduate School of Science, University of Tokyo, Japan ARTICLEINFO ABSTRACT Keywords: We describe the Belle II detector at the SuperKEKB electron–positron accelerator. SuperKEKB operates at the Belle II energy of the 훶 .4S/ resonance where pairs of B mesons are produced in a coherent quantum mechanical state Super B Factory with no additional particles. Belle II, the first Super B factory detector, aims to achieve performance comparable SuperKEKB to the original Belle and BaBar B factory experiments, which first measured the large CP violating effects in the Magnetic spectrometer B meson system, with much higher luminosity collisions and larger beam-induced backgrounds. Flavor physics Contents 1. Introduction ..................................................................................................................................................................................................... -
Lepton/Photon Highlights
sions produces two mutually oppo not be reconciled by a simple 'phase ance behaviour is in good agreement site jets, giving typical cigar-shaped space' model which assumes a with a simple quark-antiquark mod events. purely statistical decay pattern. el, the resonance decays show a As the energy is increased, one of Both theoreticians and experi totally different behaviour. these jets is seen to grow wider, but mentalists have shown vivid imagi Collinear back-to-back jets are in a very special way. Rather than nation in inventing procedures and ruled out as the dominant effect, but simply getting fatter with a cylindri names to describe this jet analysis, the data is in good agreement with a cal profile, it becomes planar, and at but the underlying structure is clear three-gluon decay model in which higher energies the jet clearly splits by simple visual inspection. Quanti the gluon fragmentation is assumed into two, giving an overall event with tative analysis is less clear-cut, but to be similar to that of a quark. Thi^ three coplanar jet components. the results of all the PETRA groups three-gluon process is the lowest The observed frequency of these are in line with QCD. order QCD contribution to the decay events agrees with quantum chro- Another scene of QCD predictions of upsilons into hadrons, and is now modynamics (QCD) calculations on is still the decay of the upsilon into clearly distinguishable from a simple the emission of hard gluons. The hadrons, as measured by PLUTO at statistical phase space description. events are incompatible with pure DORIS before its move to PETRA. -
Front-End Electronic Readout System for the Belle II Imaging Time-Of- Propagation Detector
Front-end electronic readout system for the Belle II imaging Time-Of- Propagation detector Dmitri Kotchetkova, Oskar Hartbricha,*, Matthew Andrewa, Matthew Barretta,1, Martin Bessnera, Vishal Bhardwajb,2, Thomas Browdera, Julien Cercillieuxa, Ryan Conradc, Istvan Dankod, Shawn Dubeya, James Fastc, Bryan Fulsomc, Christopher Kettera, Brian Kirbya,3, Alyssa Loosb, Luca Macchiaruloa, Boštjan Mačeka,4, Kurtis Nishimuraa, Milind Purohitb, Carl Rosenfeldb, Ziru Sanga, Vladimir Savinovd, Gary Varnera, Gerard Vissere, Tobias Webera,5, Lynn Woodc a. Department of Physics and Astronomy, University of Hawaii at Manoa, 2505 Correa Road, Honolulu, HI 96822, USA b. Department of Physics and Astronomy, University of South Carolina, 712 Main Street, Columbia, SC 29208, USA c. Pacific Northwest National Laboratory, 902 Battelle Boulevard, Richland, WA 99354, USA d. Department of Physics and Astronomy, University of Pittsburgh, 3941 O’Hara Street, Pittsburgh, PA 15260, USA e. Center for Exploration of Energy and Matter, Indiana University, 2401 North Milo B. Sampson Lane, Bloomington, IN 47408, USA * Corresponding author. Phone: 1-808-956-4097. Fax: 1-808-956-2930 E-mail address: [email protected] 1Present address: Department of Physics and Astronomy, Wayne State University, 666 W Hancock St, Detroit, MI 48201, USA 2Present address: Indian Institute of Science Education and Research Mohali, Knowledge city, Sector 81, SAS Nagar, Manauli PO 140306, India 3Present address: Physics Department, Brookhaven National Laboratory, Upton, NY 11973, USA 4Present address: Department of Experimental Particle Physics, Jožef Stefan Institute, Jamova cesta 39, 1000 Ljubljana, Slovenia 5Present address: Ruhr-Universität Bochum, 44780 Bochum, Germany Abstract The Time-Of-Propagation detector is a Cherenkov particle identification detector based on quartz radiator bars for the Belle II experiment at the SuperKEKB e+e– collider. -
Lepton Mixing and Neutrino Mass
Lepton Mixing and Neutrino Mass v Werner Rodejohann T -1 (MPIK, Heidelberg) mv = m L - m D M R m D Strasbourg MANITOP Massive Neutrinos: Investigating their July 2014 Theoretical Origin and Phenomenology 1 Neutrinos! 2 Literature ArXiv: • – Bilenky, Giunti, Grimus: Phenomenology of Neutrino Oscillations, hep-ph/9812360 – Akhmedov: Neutrino Physics, hep-ph/0001264 – Grimus: Neutrino Physics – Theory, hep-ph/0307149 Textbooks: • – Fukugita, Yanagida: Physics of Neutrinos and Applications to Astrophysics – Kayser: The Physics of Massive Neutrinos – Giunti, Kim: Fundamentals of Neutrino Physics and Astrophysics – Schmitz: Neutrinophysik 3 Contents I Basics I1) Introduction I2) History of the neutrino I3) Fermion mixing, neutrinos and the Standard Model 4 Contents II Neutrino Oscillations II1) The PMNS matrix II2) Neutrino oscillations II3) Results and their interpretation – what have we learned? II4) Prospects – what do we want to know? 5 Contents III Neutrino Mass III1) Dirac vs. Majorana mass III2) Realization of Majorana masses beyond the Standard Model: 3 types of see-saw III3) Limits on neutrino mass(es) III4) Neutrinoless double beta decay 6 Contents I Basics I1) Introduction I2) History of the neutrino I3) Fermion mixing, neutrinos and the Standard Model 7 I1) Introduction Standard Model of Elementary Particle Physics: SU(3) SU(2) U(1) C × L × Y oR +R Species # eR bR tR sR Quarks 10P 10 cR io dR i+ uR ie oL Leptons 3 13 +L eL tL Charge 3 16 cL uL bL sL dL Higgs 2 18 18 free parameters... + Gravitation + Dark Energy + Dark Matter + Baryon