Cp Violation and Flavour Mixing
Total Page:16
File Type:pdf, Size:1020Kb
Load more
Recommended publications
-
Development of an Electron Gun for the Kek Positron Generator
Particle Accelerators, 1990, Vol. 27, pp. 145-149 © 1990 Gordon and Breach, Science Publishers, Inc. Reprints available directly from the publisher Printed in the United States of America Photocopying permitted by license only DEVELOPMENT OF AN ELECTRON GUN FOR THE KEK POSITRON GENERATOR HIDEKI IWATA, YUJIRO OOAWA*, SATOSIll OHSAWA*, HITOSHI KOBAYASHI*, MITUHIRO YOKOTA*, SHIGEKI FUKUDA* and AKIRA ASAMI* Ishikawajima-harima Heavy Industries Co., Ltd. * National Laboratory for High Energy Physics(KEK) 1-1 Oho, Tsukuba-shi, Ibaraki-ken, 305 Japan Abstract In the KEK Positron Generator, a semi-long pulsed beam (-40ns) has turned out to be suitable for effective positron injection into the PF storage ring. However, to use the semi-long pulsed beam, there was a problem concerning the cathode lifetime of the gun. Thus, a new gun has been developed with a dispenser cathode, Y-796(EIMAC); the characteristics of this gun have been investigated. This new gun has been used since October 1988 and has continued to produce constant current of about 12 A without having to exchange its cathode. Thus, the cathode lifetime has been remarkably improved. INTRODUCTION Positrons had so far been utilized only in the e+-e- colliding experiments of TRISTAN, which began in November 1986. Since 1988, however, it had started to use positrons also in the Photon Factory storage ring. It had been confinned that a positron beam with a width of -40 ns was suitable for the PF ring to reduce the injection time. t ,2,3 However, to use this semi-long pulsed beam, there was a problem regarding the cathode lifetime of the old gun, the cathode of which was an oxide-coated type.4 Therefore, a new gun with a dispenser cathode, Y-796(EIMAC), has been developed to achieve a long lifetime of the cathode and to obtain a larger anode current. -
Participants
PARTICIPANTS Abbott, Richard [email protected] California Institute of Technology Aldach, Jackie [email protected] Stanford Linear Accelerator Center Allen, Christopher [email protected] Los Alamos National Laboratory Allison, Stephanie [email protected] Stanford Linear Accelerator Center Allison, Trent [email protected] Thomas Jefferson National Accelerator Facility Anicic, Damir [email protected] Paul Scherrer Institut PSI Armstrong, Dennis [email protected] Isaac Newton Group Bacher, Reinhard [email protected] DESY Backman, Raymond H. [email protected] Mega Industries, L.L.C. Baek, Sulhee [email protected] Samsung Advanced Institute of Technology Baer, Ralph C. [email protected] GSI Darmstadt Bartlett, J. Frederick [email protected] Fermi National Accelerator Laboratory Bec, Matthieu [email protected] Gemini Observatory Bernstein, Dorel [email protected] Stanford Linear Accelerator Center Bevins, Brian [email protected] Thomas Jefferson National Accelerator Facility Bickley, Matthew [email protected] Thomas Jefferson National Accelerator Facility Biocca, Alan [email protected] Lawrence Berkeley National Laboratory Birke, Thomas [email protected] Los Alamos National Laboratory PARTICIPANTS 8th International Conference on Accelerator & Large Experimental Physics Control Systems Bjorklund, Eric [email protected] Spallation Neutron Source Blumer, Thomas [email protected] Paul Scherrer Institut PSI Bolkhovityanov, Dmitry [email protected] Budker Institute of Nuclear Physics Bolshakov, Timofei [email protected] Fermi National Accelerator Laboratory Bookwalter, Valerie [email protected] Thomas Jefferson National Accelerator Facility Boriskin, Victor [email protected] Kharkov Institute Physics & Technology Bork, Rolf [email protected] California Institute of Technology Brazier, John [email protected] Brazier Systems & Consultants Ltd. -
Jongkuk Kim Neutrino Oscillations in Dark Matter
Neutrino Oscillations in Dark Matter Jongkuk Kim Based on PRD 99, 083018 (2019), Ki-Young Choi, JKK, Carsten Rott Based on arXiv: 1909.10478, Ki-Young Choi, Eung Jin Chun, JKK 2019. 10. 10 @ CERN, Swiss Contents Neutrino oscillation MSW effect Neutrino-DM interaction General formula Dark NSI effect Dark Matter Assisted Neutrino Oscillation New constraint on neutrino-DM scattering Conclusions 2 Standard MSW effect Consider neutrino/anti-neutrino propagation in a general background electron, positron Coherent forward scattering 3 Standard MSW effect Generalized matter potential Standard matter potential L. Wolfenstein, 1978 S. P. Mikheyev, A. Smirnov, 1985 D d Matter potential @ high energy d 4 General formulation Equation of motion in the momentum space : corrections R. F. Sawyer, 1999 P. Q. Hung, 2000 A. Berlin, 2016 In a Lorenz invariant medium: S. F. Ge, S. Parke, 2019 H. Davoudiasl, G. Mohlabeng, M. Sulliovan, 2019 G. D’Amico, T. Hamill, N. Kaloper, 2018 d F. Capozzi, I. Shoemaker, L. Vecchi 2018 Canonical basis of the kinetic term: 5 General formulation The Equation of Motion Correction to the neutrino mass matrix Original mass term is modified For large parameter space, the mass correction is subdominant 6 DM model Bosonic DM (ϕ) and fermionic messenger (푋푖) Lagrangian Coherent forward scattering 7 General formulation Ki-Young Choi, Eung Jin Chun, JKK Neutrino/ anti-neutrino Hamiltonian Corrections 8 Neutrino potential Ki-Young Choi, Eung Jin Chun, JKK Change of shape: Low Energy Limit: High Energy limit: 9 Two-flavor oscillation The effective Hamiltonian D The mixing angle & mass squared difference in the medium 10 Mass difference between ν&νҧ Ki-Young Choi, Eung Jin Chun, JKK I Bound: T. -
Estimation of Baryon Asymmetry of the Universe from Neutrino Physics
ESTIMATION OF BARYON ASYMMETRY OF THE UNIVERSE FROM NEUTRINO PHYSICS Manorama Bora Department of Physics Gauhati University This thesis is submitted to Gauhati University as requirement for the degree of Doctor of Philosophy Faculty of Science March 2018 I would like to dedicate this thesis to my parents . Abstract The discovery of neutrino masses and mixing in neutrino oscillation experiments in 1998 has greatly increased the interest in a mechanism of baryogenesis through leptogenesis, a model of baryogenesis which is a cosmological consequence. The most popular way to explain why neutrinos are massive but at the same time much lighter than all other fermions, is the see-saw mechanism. Thus, leptogenesis realises a highly non-trivial link between two completely independent experimental observations: the absence of antimatter in the observable universe and the observation of neutrino mixings and masses. Therefore, leptogenesis has a built-in double sided nature.. The discovery of Higgs boson of mass 125GeV having properties consistent with the SM, further supports the leptogenesis mechanism. In this thesis we present a brief sketch on the phenomenological status of Standard Model (SM) and its extension to GUT with or without SUSY. Then we review on neutrino oscillation and its implication with latest experiments. We discuss baryogenesis via leptogenesis through the decay of heavy Majorana neutrinos. We also discuss formulation of thermal leptogenesis. At last we try to explore the possibilities for the discrimination of the six kinds of Quasi- degenerate neutrino(QDN)mass models in the light of baryogenesis via leptogenesis. We have seen that all the six QDN mass models are relevant in the context of flavoured leptogenesis. -
Neutrinos and Beyond — Opening a New Era of Cosmic-Ray Research
ADVERTISEMENT FEATURE THE UNIVERSITY OF TOKYO Neutrinos and beyond — Opening a new era of cosmic-ray research Takaaki Kajita, a recipient of the 2015 that neutrinos are massless. These discov- Nobel Prize in Physics, and other re- eries, which resulted in Kajita’s 2015 Nobel searchers at the University of Tokyo’s Prize in Physics, were made a team led by Institute for Cosmic Ray Research (ICRR) him in 1998. have been exploring new realms in par- Kajita acknowledged his success owed ticle physics research. Kajita’s work on a lot to the strong support he received neutrinos and related research at ICRR from two mentors and former supervisors is leading the world in this field. — Masatoshi Koshiba and Yoji Totsuka. Koshiba was awarded the 2002 Nobel Prize The path to a Nobel prize in Physics for detecting neutrinos pro- Particle physics and astrophysics are duced in supernovae using Kamiokande, among the most active research fields at the predecessor of Super-Kamiokande. the University of Tokyo, and its Institute for Totsuka led the Super-Kamiokande proj- Cosmic Ray Research (ICRR) is leading the ect as Koshiba’s successor. Totsuka’s con- world with explorations in these areas. ICRR tribution was so great that many believe is best known for its research on neutrinos he would have shared the Nobel Prize with using the world’s largest underground neu- Kajita if he were alive. trino detector, Super-Kamiokande. The de- Kajita’s award-winning work dates tector is located in a mine in central Japan back to 1986 when he earned his PhD for and is filled with 50,000 tons of pure water. -
FROM KEK-PS to J-PARC Yoshishige Yamazaki, J-PARC, KEK & JAEA, Japan
FROM KEK-PS TO J-PARC Yoshishige Yamazaki, J-PARC, KEK & JAEA, Japan Abstract target are located in series. Every 3 s or so, depending The user experiments at J-PARC have just started. upon the usage of the main ring (MR), the beam is JPARC, which stands for Japan Proton Accelerator extracted from the RCS to be injected to the MR. Here, it Research Complex, comprises a 400-MeV linac (at is ramped up to 30 GeV at present and slowly extracted to present: 180 MeV, being upgraded), a 3-GeV rapid- Hadron Experimental Hall, where the kaon-production cycling synchrotron (RCS), and a 50-GeV main ring target is located. The experiments using the kaons are (MR) synchrotron, which is now in operation at 30 GeV. conducted there. Sometimes, it is fast extracted to The RCS will provide the muon-production target and the produce the neutrinos, which are sent to the Super spallation-neutron-production target with a beam power Kamiokande detector, which is located 295-km west of of 1 MW (at present: 120 kW) at a repetition rate of 25 the J-PARC site. In the future, we are conceiving the Hz. The muons and neutrons thus generated will be used possibility of constructing a test facility for an in materials science, life science, and others, including accelerator-driven nuclear waste transmutation system, industrial applications. The beams that are fast extracted which was shifted to Phase II. We are trying every effort from the MR generate neutrinos to be sent to the Super to get funding for this facility. -
QUANTUM GRAVITY EFFECT on NEUTRINO OSCILLATION Jonathan Miller Universidad Tecnica Federico Santa Maria
QUANTUM GRAVITY EFFECT ON NEUTRINO OSCILLATION Jonathan Miller Universidad Tecnica Federico Santa Maria ARXIV 1305.4430 (Collaborator Roman Pasechnik) !1 INTRODUCTION Neutrinos are ideal probes of distant ‘laboratories’ as they interact only via the weak and gravitational forces. 3 of 4 forces can be described in QFT framework, 1 (Gravity) is missing (and exp. evidence is missing): semi-classical theory is the best understood 2 38 2 graviton interactions suppressed by (MPl ) ~10 GeV Many sources of astrophysical neutrinos (SNe, GRB, ..) Neutrino states during propagation are different from neutrino states during (weak) interactions !2 SEMI-CLASSICAL QUANTUM GRAVITY Class. Quantum Grav. 27 (2010) 145012 Considered in the limit where one mass is much greater than all other scales of the system. Considered in the long range limit. Up to loop level, semi-classical quantum gravity and effective quantum gravity are equivalent. Produced useful results (Hawking/etc). Tree level approximation. gˆµ⌫ = ⌘µ⌫ + hˆµ⌫ !3 CLASSICAL NEUTRINO OSCILLATION Neutrino Oscillation observed due to Interaction (weak) - Propagation (Inertia) - Interaction (weak) Neutrino oscillation depends both on production and detection hamiltonians. Neutrinos propagates as superposition of mass states. 2 2 2 mj mk ∆m L iEat ⌫f (t) >= Vfae− ⌫a > φjk = − L = | | 2E⌫ 4E⌫ a X 2 m m2 i j L i k L 2E⌫ 2E⌫ P⌫f ⌫ (E,L)= Vf 0jVf 0ke− e Vfj⇤ Vfk⇤ ! f0 j,k X !4 MATTER EFFECT neutrinos interact due to flavor (via W/Z) with particles (leptons, quarks) as flavor eigenstates MSW effect: neutrinos passing through matter change oscillation characteristics due to change in electroweak potential effects electron neutrino component of mass states only, due to electrons in normal matter neutrino may be in mass eigenstate after MSW effect: resonance Expectation of asymmetry for earth MSW effect in Solar neutrinos is ~3% for current experiments. -
Quantum Mechanics Quantum Chromodynamics (QCD)
Quantum Mechanics_quantum chromodynamics (QCD) In theoretical physics, quantum chromodynamics (QCD) is a theory ofstrong interactions, a fundamental forcedescribing the interactions between quarksand gluons which make up hadrons such as the proton, neutron and pion. QCD is a type of Quantum field theory called a non- abelian gauge theory with symmetry group SU(3). The QCD analog of electric charge is a property called 'color'. Gluons are the force carrier of the theory, like photons are for the electromagnetic force in quantum electrodynamics. The theory is an important part of the Standard Model of Particle physics. A huge body of experimental evidence for QCD has been gathered over the years. QCD enjoys two peculiar properties: Confinement, which means that the force between quarks does not diminish as they are separated. Because of this, when you do split the quark the energy is enough to create another quark thus creating another quark pair; they are forever bound into hadrons such as theproton and the neutron or the pion and kaon. Although analytically unproven, confinement is widely believed to be true because it explains the consistent failure of free quark searches, and it is easy to demonstrate in lattice QCD. Asymptotic freedom, which means that in very high-energy reactions, quarks and gluons interact very weakly creating a quark–gluon plasma. This prediction of QCD was first discovered in the early 1970s by David Politzer and by Frank Wilczek and David Gross. For this work they were awarded the 2004 Nobel Prize in Physics. There is no known phase-transition line separating these two properties; confinement is dominant in low-energy scales but, as energy increases, asymptotic freedom becomes dominant. -
Scaling Laws in Particle Physics and Astrophysics
SCALING LAWS IN PARTICLE PHYSICS AND ASTROPHYSICS RUDOLF MURADYAN Dedicated to the Golden Jubilee (1961-2011) of publication of the article by Geoffrey Chew and Steven Frautschi in Phys. Rev. Lett. 7, 394, 1961, where a celebrated scaling law J m2 has been conjectured for spin/mass dependence of hadrons. G. Chew S. Frautschi 1. INTRODUCTION: WHAT IS SCALING? Any polynomial power law f() x c xn , where constant c has a dimension dim f dimc (dimx )n exhibits the property of scaling or scale invariance. Usually n is called scaling exponent. The word scaling express the fact that function f is shape-invariant with respect to the dilatation transformation x x f ( x) c ( x)n n f() x and this transformation preserves the shape of function f . We say, following Leonhard Euler, that f is homogeneous of degree “n” if for any value of parameter f ( x) n f() x . Differentiating this relation with respect to and putting 1we obtain simple differential equation x f() x n f() x solution of which brings back to the polynomial power scaling law. There are tremendously many different scaling laws in Nature. The most important of them can be revealed by Google search of scaling site:nobelprize.org in the official site of Nobel Foundation, where nearly 100 results appears. Ten of them are shown below: 1. Jerome I. Friedman - Nobel Lecture 2. Daniel C. Tsui - Nobel Lecture 3. Gerardus 't Hooft - Nobel Lecture 4. Henry W. Kendall - Nobel Lecture 5. Pierre-Gilles de Gennes - Nobel Lecture 6. Jack Steinberger - Nobel Lecture 7. -
Baryogenesis and Dark Matter from B Mesons: B-Mesogenesis
Baryogenesis and Dark Matter from B Mesons: B-Mesogenesis Miguel Escudero Abenza [email protected] arXiv:1810.00880, PRD 99, 035031 (2019) with: Gilly Elor & Ann Nelson Based on: arXiv:2101.XXXXX with: Gonzalo Alonso-Álvarez & Gilly Elor New Trends in Dark Matter 09-12-2020 The Universe Baryonic Matter 5% 26% Dark Matter 69% Dark Energy Planck 2018 1807.06209 Miguel Escudero (TUM) B-Mesogenesis New Trends in DM 09-12-20 !2 Theoretical Understanding? Motivating Question: What fraction of the Energy Density of the Universe comes from Physics Beyond the Standard Model? 99.85%! Miguel Escudero (TUM) B-Mesogenesis New Trends in DM 09-12-20 !3 SM Prediction: Neutrinos 40% 60% Photons Miguel Escudero (TUM) B-Mesogenesis New Trends in DM 09-12-20 !4 The Universe Baryonic Matter 5% 26% Dark Matter 69% Dark Energy Planck 2018 1807.06209 Miguel Escudero (TUM) B-Mesogenesis New Trends in DM 09-12-20 !5 Baryogenesis and Dark Matter from B Mesons: B-Mesogenesis arXiv:1810.00880 Elor, Escudero & Nelson 1) Baryogenesis and Dark Matter are linked 2) Baryon asymmetry directly related to B-Meson observables 3) Leads to unique collider signatures 4) Fully testable at current collider experiments Miguel Escudero (TUM) B-Mesogenesis New Trends in DM 09-12-20 !6 Outline 1) B-Mesogenesis 1) C/CP violation 2) Out of equilibrium 3) Baryon number violation? 2) A Minimal Model & Cosmology 3) Implications for Collider Experiments 4) Dark Matter Phenomenology 5) Summary and Outlook Miguel Escudero (TUM) B-Mesogenesis New Trends in DM 09-12-20 !7 Baryogenesis -
Neutrino Physics
SLAC Summer Institute on Particle Physics (SSI04), Aug. 2-13, 2004 Neutrino Physics Boris Kayser Fermilab, Batavia IL 60510, USA Thanks to compelling evidence that neutrinos can change flavor, we now know that they have nonzero masses, and that leptons mix. In these lectures, we explain the physics of neutrino flavor change, both in vacuum and in matter. Then, we describe what the flavor-change data have taught us about neutrinos. Finally, we consider some of the questions raised by the discovery of neutrino mass, explaining why these questions are so interesting, and how they might be answered experimentally, 1. PHYSICS OF NEUTRINO OSCILLATION 1.1. Introduction There has been a breakthrough in neutrino physics. It has been discovered that neutrinos have nonzero masses, and that leptons mix. The evidence for masses and mixing is the observation that neutrinos can change from one type, or “flavor”, to another. In this first section of these lectures, we will explain the physics of neutrino flavor change, or “oscillation”, as it is called. We will treat oscillation both in vacuum and in matter, and see why it implies masses and mixing. That neutrinos have masses means that there is a spectrum of neutrino mass eigenstates νi, i = 1, 2,..., each with + a mass mi. What leptonic mixing means may be understood by considering the leptonic decays W → νi + `α of the W boson. Here, α = e, µ, or τ, and `e is the electron, `µ the muon, and `τ the tau. The particle `α is referred to as the charged lepton of flavor α. -
Peering Into the Universe and Its Ele Mentary
A gigantic detector to explore elementary particle unification theories and the mysteries of the Universe’s evolution Peering into the Universe and its ele mentary particles from underground Ultrasensitive Photodetectors The planned Hyper-Kamiokande detector will consist of an Unified Theory and explain the evolution of the Universe order of magnitude larger tank than the predecessor, Super- through the investigation of proton decay, CP violation (the We have been developing the world’s largest photosensors, which exhibit a photodetection Kamiokande, and will be equipped with ultra high sensitivity difference between neutrinos and antineutrinos), and the efficiency two times greater than that of the photosensors. The Hyper-Kamiokande detector is both a observation of neutrinos from supernova explosions. The Super-Kamiokande photosensors. These new “microscope,” used to observe elementary particles, and a Hyper-Kamiokande experiment is an international research photosensors are able to perform light intensity “telescope”, used to study the Sun and supernovas through project aiming to become operational in the second half of and timing measurements with a much higher neutrinos. Hyper-Kamiokande aims to elucidate the Grand the 2020s. precision. The new Large-Aperture High-Sensitivity Hybrid Photodetector (left), the new Large-Aperture High-Sensitivity Photomultiplier Tube (right). The bottom photographs show the electron multiplication component. A megaton water tank The huge Hyper-Kamiokande tank will be used in order to obtain in only 10 years an amount of data corresponding to 100 years of data collection time using Super-Kamiokande. This Experimental Technique allows the observation of previously unrevealed The photosensors on the tank wall detect the very weak Cherenkov rare phenomena and small values of CP light emitted along its direction of travel by a charged particle violation.