DOCSLIB.ORG

Neutrino Experiments

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
Neutrino Experiments Neutrino Experiments 1. Neutrinos and n observatories 2. Establishing n oscillation & mixing 3. Present questions and experiments Sofia Andringa, LIP July 2017 17th JINR-ISU Baikal Summer School on Physics of Elementary Particles and Astrophysics What are neutrinos? 1, 2, 3 n Neutrino n sources detection 1. Neutrinos and n observatories Discovery of neutrino oscillations the elementary particles g . g . W,Z Neutrino masses not to scale: == ZERO in the Standard Model what are neutrinos? 1930: an “undetected particle” ensuring energy conservation in b-decays (Pauli) Dear Radioactive Ladies and Gentlemen, (...) I have hit upon a desperate remedy to save (...) the law of energy conservation. (...) emitted together with the electron, in such a way that the sum of the energies (...) is constant. (...) electrically neutral particles (...) s n (Z,A) –> (Z+1,A) + b mass not larger than 0.01 proton mass(...) o r t c M(Z,A) = M(Z+1,A) + E e (...) the question concerning experimental proof of l e n –> p + e⁻ + v such a neutron, if it has something like about 10 times n i the penetrating capacity of a g -ray. y t i s n e t n I Electron kinetic energy (MeV) “inverse beta decay” 1934: Fermi, “attempt at a theory of b rays” weak interaction (GF~10⁻⁵ GeV ⁻ ²) cross-section ~ 10⁻⁴⁴ cm² for E ~ MeV mean free path of 10¹⁹ m in water or 1 out of 10¹⁹ interact in 1m of water need both a large number of neutrinos and a large number of targets (electron anti-)neutrinos detected 25 years after first proposal the Reines and Cowen experiment delayed coincidences in liquid scintilator Reines nobel lecture(1995) to detect neutrinos from nuclear reactors electron / muon / neutrino p -> mn -> enn are all the neutrinos the same? 3 types of detectable neutrinos Electron neutrino (1956) Muon neutrino (1962) (by Lederman, Steinberg & Schwartz, at BNL) following suggestion by B. Pontecorvo (1960) Tau neutrino (2000) (by DONUT, at Fermilab) following the discovery of the tau lepton (1975), the bottom quark (1977), and the top quark (1995) measuring 3 undetected neutrinos 3 neutrinos (m<45 GeV) @ LEP nx Z nx all neutrinos are missing ET @ LHC neutral and charged interactions Neutrino is not seen n but transfers energy to matter Lepton of the same family Z⁰ n E > m=511 keV, e W 106 MeV, m 1.78 GeV, t ICARUS (Lar TPC) @ CNGS, nm with E=17 GeV interactions increase with energy nm n, m Z,W (Quasi)Elastic to Deep Inelastic N(p, n) p, n, p, D -> pp / pn, many p, ... K2K 1 GeV interaction cross-section sources of neutrinos ~ 30 orders of magnitude detected Geo anti-neutrino 3 x 113 / cm³ observations Geo (Borexino) SN1987A (Kamioka-II) Astro (IceCube) Sun (SuperK) neutrino detector requirements Large and uniform target for neutrino interaction Sensitive detection medium for produced particles Transparent for signal propagation (usually the signal is light) Baikal Good efficiency and high coverage for (light) signal detection + Low background environment shielded from cosmic rays (and radioactivity at low E) ... water is one of the favorite media underground telescopes 1967 – start of construction 1977 – BUST (SN1987A n) Baksan Underground Scintillator Telescope 11m x 280 m² 3180 detectors, 330 tons of liquid scint. 1987 – SAGE (Solar pp n) Soviet-American Gallium Experiment 50 tons of liquid Ga 2017 – being extended detecting Supernovae a Supernova explodes in the Large Magallean Cloud and SNEWS in February 23rd 1987 it is even visible with naked high Neutrino observatories saw coincident events, three hours before! Baksan Underground Scintillator Telescope KamiokaNDE 4-level building, 11m x 280 m² Nucleon Decay Experiment in Japan 3180 detectors, 330 tons of liquid scint. observing protons in 1 kton of water monitoring the Sun with neutrinos SAGE: n + Ga(31p,40n) --> Ge(32p,39n) main nuclear fusion process 50 tons of liquid Ga, 15 Ge atoms/month in the Sun is 2e⁻ + 4p -> ⁴He + 2 n + 27 MeV n g ~60% of the expected rate!! from measured luminosity: ~ 60 billion n / (cm² s) [exercise: calculate Solar flux] something wrong with the Sun? Counting at low energy with inverse b⁺ decay ⁷¹Ga -> ⁷¹Ge (E>0.2 MeV): => 60% of expected fluxes ³⁷ Cl -> ³ ⁷ Ar (E>0.8 MeV) => 30% of expected fluxes Seeing with “n-e scattering” => 50% of expected fluxes SN1987A detection && the solar neutrino problem lead to new experiments the new water Cherenkov detectors the Super Kamiokande 1000 m underground in Japan 50,000 ton of pure water + 2 000 in OD) ｍ 11,000 PMT 50 cm ( ２ ４ ３９ｍ the Sudbury Neutrino Observatory 2000 m underground in Canada 1,000 ton of (salted) heavy water 9,000 PMT 50 cm (+ 90 in OD) 20 ｍ the new water Cherenkov detectors the Super Kamiokande 1000 m underground in Japan 50,000 ton of pure water 11,000 PMT 50 cm (+ 2 000 in OD) the Super Kamiokande detector Cherenkov detectors Cherenkov effect PMTs velocity higher than ... SKI 1996-2001 SKII 2002-2005 (50% PMTs) SKIII 2006-2008 (100% PMTs) SKIV 2009-now (new electronics) KamiokaNDE II saw SN1987A, now discussing HiperKamiokande solar neutrinos in water 500 days and nights of exposure to Sun Flux is one half of what is expected from the Standard Solar Model Constant along years and seasons, equal during day and night (*) the new water Cherenkov detectors the Sudbury Neutrino Observatory 2000 m underground in Canada 1,000 ton of (salted) heavy water 9,000 PMT 50 cm (+ 90 in OD) Three different phases with different neutron capture efficiency: I – capture in D2O; II – in Salt (Cl*); III – in dedicated counters 20 ｍ the Sudbury Neutrino Obsevatory located 2000 m underground In a still active nickel mine lots of heavy water in Canada solar neutrinos in (salted) heavy water 1) Electron scattering (as in H2O) n + e -> n + e (only 0.50 x SSM) instead of mixing neutrino types SNO can count them separately! [exercise: Feynman diagrams] 2) Charged Current, only ne 3) Neutral Current, all nx separating n counts in SNO radius Very low background in inner volume ES pointing to the Sun, confirms SK CC (one ring) vs NC (more rings) Normalization of the 4 components direction isotropy solution of the solar neutrino problem NC (all neutrinos) = 1.00 x Solar Model CC (ne) / NC (nx) = 0.35 the Sun is well! neutrinos change between production in the Sun and detection at Earth neutrinos must have mass 1 SNU = 10⁻ ³ ⁶ captures / atom /second n from Nature @ Super Kamiokande 500 days + nights exposure Flux lower than Solar ne Solar ne @ MeV Atmospheric ne ne nm nm @ GeV higher energy but lower flux nm / ne ~ 2 in all directions GeV events at Super Kamiokande nl l = e, m (t), n p, n, p,... p0 -> gg ep0 identifying electrons and muons l = e, m nl kinematics of e/m give n energy and direction no charge measurement muon neutrino disappearence p -> nm m -> nm nm ne e nm / ne ~ 2 Fluxes confirmed by ne 10 km cosq =1 10 000 km cosq =-1 first measurement of n oscillations expected from cosmic ray fluxes confirmed by electron measurements fit with 1 - sin²2q sin²(1.27 Dm² L/E) @GeV 1 10 100 1000 km first measurement of n oscillations nt new 1 - sin²2q sin²(1.27 Dm² L/E) results maximal amplitude at L ~ 500 km / E ~ 1 GeV Dm² ~ 10⁻ ³ eV² No time to change Fast m-t change @GeV 1 10 100 1000 km two neutrino oscillations Amplitude Frequency |Va> cosq sinq |V1> [ |V >]=[ -sin cos ][|V >] b q q 2 |V(0)> = |Va> = cosq |V1> + sinq |V2> |V(t )> = cosq exp[-i (E1 t – p1 x)] |V1> + sinq exp[-i (E2 t – p2 x)] |V2> 2 2 2 2 2 P=|<Vb(t)|Va>|² with L = ct Ei = p + mi ~ (p + mi /2E) oscillations and mass l (E, M) E²=P²+M² F = (Mx²-My²)/E For propagation, only energy and mass are relevant L = c.Time For interaction, only the energy and flavor are relevant Each mass has a combination of different interaction flavors and each flavor has a combination of the different masses Ve Vm Vt Mx and My at production and detection L = c.Time (interaction in dense matter can be seen as inducing an effective mass).
Load more

Recommended publications
  • The History of Neutrinos, 1930 − 1985
    The History of Neutrinos, 1930 − 1985. What have we Learned About Neutrinos? What have we Learned Using Neutrinos? J. Steinberger Prepared for “25th International Conference On Neutrino Physics and Astrophysics”, Kyoto (Japan), June 2012 1 2 3 4 The detector of the experiment of Conversi, Pancini and Piccioni, 1946, 5 which showed that the mesotron is not the Yukawa particle. Detector with 80 Geiger counters. The muon decay spectrum is continuous. My thesis experiment, under Fermi, which showed that the muon decays into two neutral particles, plus the electron. Fermi, myself and others, in 1954, at a summer school in Varenna, lake Como, a few months before Fermi’s untimely disappearance. 6 Demonstration of the Neutrino In 1956 Cowan and Reines detected antineutrinos from a nuclear reactor, reacting with protons in liquid scintillator which also contained cadmium, observing the positron as well as the scattering of the neutron on cadmium. 7 The Electron and Muon Neutrinos are Different. 1. G. Feinberg, 1958. 2. B. Pontecorvo, 1959. 3. M. Schwartz (T.D. Lee), 1959 4. Higher energy accelerators, Courant, Livingston and Snyder. Pontecorvo 8 9 A C B D Spark chamber and counter arrangement. A are triggering counters, Energy spectra of neutrinos B, C and D are anticoincidence counters from pion and kaon decays. 10 Event with penetrating muon and hadron shower 11 The group of the 2nd neutrino experiment in 1962: J.S., Goulianos, Gaillard, Mistry, Danby, technician whose name I have forgotten, Lederman and Schwartz. 12 Same group, 26 years later, at Nobel ceremony in Stockholm. 13 Discovery of partons, nucleon structure, scaling, in deep inelastic scattering of electrons on protons at SLAC in 1969.
    [Show full text]
  • Neutrino Physics
    Neutrino Physics Steve Boyd University of Warwick Course Map 1. History and properties of the neutrino, neutrino interactions, beams and detectors 2. Neutrino mass, direct mass measurements, double beta decay, flavour oscillations 3. Unravelling neutrino oscillations experimentally 4. Where we are and where we're going References K. Zuber, “Neutrino Physics”, IoP Publishing 2004 C. Giunti and C.W.Kim, “Fundamentals of Neutrino Physics and Astrophysics”, Oxford University Press, 2007. R. N. Mohaptara and P. B. Pal, “Massive Neutrinos in Physics and Astrophysics”, World Scientific (2nd Edition), 1998 H.V. Klapdor-Kleingrothaus & K. Zuber, “Particle Astrophysics”,IoP Publishing, 1997. Two Scientific American articles: “Detecting Massive Neutrinos”, E. Kearns, T. Kajita, Y. Totsuka, Scientific American, August 1999. “Solving the Solar Neutrino Problem”, A.B. McDonald, J.R. Klein, D.L. Wark, Scientific American, April 2003. Plus other Handouts Lecture 1 In which history is unravelled, desperation is answered, and the art of neutrino generation and detection explained Crisis It is 1914 – the new study of atomic physics is in trouble (Z+1,A) Spin 1/2 (Z,A) Spin 1/2 Spin 1/2 electron Spin ½ ≠ spin ½ + spin ½ E ≠ E +e Ra Bi “At the present stage of atomic “Desperate remedy.....” theory we have no arguments “I do not dare publish this idea....” for upholding the concept of “I admit my way out may look energy balance in the case of improbable....” b-ray disintegrations.” “Weigh it and pass sentence....” “You tell them. I'm off to a party” Detection of the Neutrino 1950 – Reines and Cowan set out to detect n 1951 1951 1951 I.
    [Show full text]
  • Dstau: Study of Tau Neutrino Production with 400 Gev Protons from the CERN-SPS
    Prepared for submission to JHEP DsTau: Study of tau neutrino production with 400 GeV protons from the CERN-SPS Shigeki Aoki,a Akitaka Ariga,b;1 Tomoko Ariga,b;c Sergey Dmitrievsky,d Elena Firu,e Dean Forshaw,b Tsutomu Fukuda,f Yuri Gornushkin,d Ali Murat Guler,g Maria Haiduc,e Koichi Kodama,h Masahiro Komatsu,f Muhtesem Akif Korkmaz,g Umut Kose,i Madalina Miloi,e Antonio Miucci,b Motoaki Miyanishi,f Mitsuhiro Nakamura,f Toshiyuki Nakano,f Alina Neagu,e Hiroki Rokujo,f Osamu Sato,f Elizaveta Sitnikova,d Yosuke Suzuki,f Tomoki Takao,f Svetlana Vasina,d Mykhailo Vladymyrov,b Thomas Weston,b Junya Yoshida,j Masahiro Yoshimoto.k The DsTau Collaboration aKobe University, Kobe, Japan bAlbert Einstein Center for Fundamental Physics, Laboratory for High Energy Physics, University of Bern, Bern, Switzerland cKyushu University, Fukuoka, Japan dJoint Institute for Nuclear Research, Dubna, Russia eInstitute of Space Science, Bucharest, Romania f Nagoya University, Nagoya, Japan gMiddle East Technical University, Ankara, Turkey hAichi University of Education, Kariya, Japan iCERN, Geneva, Switzerland jAdvanced Science Research Center, Japan Atomic Energy Agency, Tokai, Japan kGifu University, Gifu, Japan E-mail: [email protected] Abstract: In the DsTau experiment at the CERN SPS, an independent and direct way to measure tau neutrino production following high energy proton interactions was proposed. As the main source of tau neutrinos is a decay of Ds mesons, produced in proton-nucleus arXiv:1906.03487v1 [hep-ex] 8 Jun 2019 interactions, the project aims at measuring a differential cross section of this reaction. The experimental method is based on a use of high resolution emulsion detectors for effective registration of events with short lived particle decays.
    [Show full text]
  • HARP Targets Pion Production Cross Section and Yield Measurements: Implications for Miniboone Neutrino Flux
    HARP targets pion production cross section and yield measurements: Implications for MiniBooNE neutrino flux A Dissertation Submitted to the Graduate School of the University of Cincinnati in partial fulfillment of the requirements for the degree of Doctor of Philosophy in the Department of Physic of the College of Arts and Sciences July 2015 by Don Athula Abeyarathna Wickremasinghe M.Sc., University of Cincinnati, 2011 M.Sc., Norwegian University of Science and Technology (NTNU), 2008 B.Sc., University of Peradeniya, 2002 Committee Chair: Professor Randy A. Johnson © 2015 Don Athula A. Wickremasinghe All Rights Reserved HARP targets pion production cross section and yield measurements: Implications for MiniBooNE neutrino flux Don Athula Abeyarathna Wickremasinghe Abstract The prediction of the muon neutrino flux from a 71.0 cm long beryllium target for the MiniBooNE experiment is based on a measured pion production cross section which was taken from a short beryllium target (2.0 cm thick - 5% nuclear interaction length) in the Hadron Production (HARP) experiment at CERN. To verify the extrapolation to our longer target, HARP also measured the pion production from 20.0 cm and 40.0 cm beryllium targets. The measured production yields, d2N π± (p; θ)=dpdΩ, on targets of 50% and 100% nuclear interaction lengths in the kinematic rage of momentum from 0.75 GeV/c to 6.5 GeV/c and the range of angle from 30 mrad to 210 mrad are presented along with an update of the short target cross sections. The best fitted extended Sanford-Wang (SW) model parameterization for updated short beryllium target π+ production cross section is presented.
    [Show full text]
  • Pos(Nufact2017)067 Mass Range
    Neutrino cross-section measurement prospects with SBND PoS(NuFact2017)067 Nicola McConkey∗ for the SBND Collaboration University of Sheffield E-mail: [email protected] SBND (Short-Baseline Near Detector) is a 112ton liquid argon time projection chamber (LArTPC) neutrino detector under construction in the Fermilab Booster Neutrino Beam. Together with MicroBooNE and ICARUS-T600 detectors, SBND will search for short baseline neutrino oscillations in the 1eV2 mass range. SBND will also perform detailed studies of the physics of neutrino-argon interactions, thanks to a data sample of millions of electron and muon neutrino interactions. Finally SBND plays an important role in the on-going R&D effort to develop the LArTPC technology, testing several technologies that can be used in a future kiloton-scale neu- trino detectors for a long-baseline experiment. We will discuss the detector design, its current status, and the physics program, with a particular focus on the neutrino cross-section measure- ment prospects. The 19th International Workshop on Neutrinos from Accelerators-NUFACT2017 25-30 September, 2017 Uppsala University, Uppsala, Sweden ∗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). https://pos.sissa.it/ Neutrino cross-section measurement prospects with SBND Nicola McConkey Table 1: Parameters of the three SBN detectors. Detector Baseline (m) Active LAr mass (tonnes) SBND 110 112 MicroBooNE 470 87 ICARUS T-600 600 476 1. Introduction Over the past 20 years there have been several experimental anomalies observed in neutrino PoS(NuFact2017)067 experiments with baselines of the order of <1km, which are referred to as short baseline exper- iments.
    [Show full text]
  • A Study of Systematic Uncertainties for a Photon-Like Low Energy Excess Search at Microboone
    University of Tennessee, Knoxville TRACE: Tennessee Research and Creative Exchange Doctoral Dissertations Graduate School 8-2021 A Study of Systematic Uncertainties for a Photon-like Low Energy Excess Search at MicroBooNE Gray Yarbrough [email protected] Follow this and additional works at: https://trace.tennessee.edu/utk_graddiss Part of the Elementary Particles and Fields and String Theory Commons, and the Plasma and Beam Physics Commons Recommended Citation Yarbrough, Gray, "A Study of Systematic Uncertainties for a Photon-like Low Energy Excess Search at MicroBooNE. " PhD diss., University of Tennessee, 2021. https://trace.tennessee.edu/utk_graddiss/6575 This Dissertation is brought to you for free and open access by the Graduate School at TRACE: Tennessee Research and Creative Exchange. It has been accepted for inclusion in Doctoral Dissertations by an authorized administrator of TRACE: Tennessee Research and Creative Exchange. For more information, please contact [email protected]. To the Graduate Council: I am submitting herewith a dissertation written by Gray Yarbrough entitled "A Study of Systematic Uncertainties for a Photon-like Low Energy Excess Search at MicroBooNE." I have examined the final electronic copy of this dissertation for form and content and recommend that it be accepted in partial fulfillment of the equirr ements for the degree of Doctor of Philosophy, with a major in Physics. Sowjanya Gollapinni, Major Professor We have read this dissertation and recommend its acceptance: Stefan M Spanier, Nadia Fomin, David C Donovan Accepted for the Council: Dixie L. Thompson Vice Provost and Dean of the Graduate School (Original signatures are on file with official studentecor r ds.) A Study of Systematic Uncertainties for a Photon-like Low Energy Excess Search at MicroBooNE A Dissertation Presented for the Doctor of Philosophy Degree The University of Tennessee, Knoxville Gray Yarbrough August 2021 © by Gray Yarbrough, 2021 All Rights Reserved.
    [Show full text]
  • Neutrinos: Dirac Or Majorana?
    Neutrinos: Dirac or Majorana? Dirac Majorana How to address Dirac vs. Majorana question? ❏ 흂 ≠ 흂̅ ❏ 흂 = 흂̅ ❏ Find exception to the property that a Majorana ❏ LNC ❏ LNV neutrino behaves almost like a Dirac one. Dirac vs. Majorana: Why should we care? E.g., kaon/pion decays to heavy neutrino. ❏ Origin of neutrino masses and mixings ❏ Find an effective way of working with ❏ If Majorana, possible explanation for the non-relativistic neutrinos. matter-antimatter asymmetry E.g., the relic neutrinos from the Big Bang. ❏ Neutrinos have been full of surprises. ❏ Find some process that addresses the question even though it does not involve neutrinos at all. Why determining this is very challenging? E.g., Neutrinoless double beta decay. ❏ When a neutrino is ultra-relativistic, its behavior is insensitive to its nature. Neutrinos: Dirac or Majorana? The most promising approach Other approaches ❏ 0νββ: observation of 0νββ would imply ❏ Capture the relic neutrinos from the Big Bang on Majorana nature of neutrino. tritium The total capture rate is two times larger in the Majorana case compared to that in the Dirac one. ❏ (Heavy) neutrino decays: N → ν + X Angular distribution of X in the N’s rest frame: isotropic if Majorana, almost never isotropic if Dirac. Physics Letters B 789 (2019) 488-495 ❏ Many more … E.g., LNV at LHC and ee collider. Pion Decay to Heavy Neutrinos https://arxiv.org/abs/1805.00922 Suppose there is a fourth neutrino mass Dirac N: state which has some coupling to the ● Lepton number conservation means weak flavor states. Consider
    [Show full text]
  • Isbn-13: 978-1-4392-4118-9 Isbn-10: 1-4392-4118-X
    ISBN-13: 978-1-4392-4118-9 ISBN-10: 1-4392-4118-X (6-26-09) Page 1 of 89 © 2009 Faith in the Future Foundation www.apocalypse2008-2015.com A Donut Atom Nuclear Story Table of Contents Page # 3 Foreword to A Donut Nuclear Story - Section 5 37 Explaining a New Donut Atom Model 6 The Mechanism Sustaining the Universe A Mini-Babushka Egg Summary of the Donut Model 6 A Donut Transformer 37 Galaxy Pictures Demonstrate the Donut Atom Model 8 Kelvin Temperature 37 - Section 1 9 A Transformer Pendulum 40 A New Concept of Atomic Structure A Divine Intelligence Transformer 40 Introduction 9 A Chinese Binary Code Explained 41 Donut Atom Model Proposal 10 How are Neutrons Controlled? 42 - ”Love Code, a twist of light only mantis shrimp can Section 2 11 43 Groundwork for a New Theory see” An Antikythera clock fits the Rainbow Pendulum 43 A Mystery Rainbow Above God’s throne 11 System Rainbow Spectrum Lines Part 1 12 Did God Slow Down the Time Pendulum? 43 What Scientists Learn From Spectrums 12 Infinite Energy Dispenser Principle 44 A New Math Equation 14 The Cuckoo Clock in Heaven 45 Energy Scalability Explained 14 - Proposed Entropy Laws of the Universe 15 Section 6 46 Ancient Clocks Connect with Donut Atoms 15 Why do we have a Universe? More Proof that Light is Slowing Down 19 An Expanding, Dynamic Universe 46 Is Time Literally Slowing Down and Disappearing A Static Universe Frozen in Time 47 21 From the Universe? Processes Forming the Universe 47 Do the Laws of Nature Change with Time? 21 [Neutrino-Neutron] vs.
    [Show full text]
  • Measurement of Neutrino Oscillations in Atmospheric Neutrinos with the Icecube Deepcore Detector
    Measurement of neutrino oscillations in atmospheric neutrinos with the IceCube DeepCore detector Dissertation zur Erlangung des akademischen Grades doctor rerum naturalium ( Dr. rer. nat.) im Fach Physik eingereicht an der Mathematisch-Naturwissenschafltichen Fakultät I der Humboldt-Universität zu Berlin von B.Sc. Juan Pablo Yáñez Garza Präsident der Humboldt-Universität zu Berlin: Prof. Dr. Jan-Hendrik Olbertz Dekan der Mathematisch-Naturwissenschaftlichen Fakultät I: Prof. Stefan Hecht, Ph.D. Gutachter: 1. Prof. Dr. Hermann Kolanoski 2. Prof. Dr. Allan Halgren 3. Prof. Dr. Thomas Lohse Tag der mündlichen Prüfung: 02.06.2014 iii Abstract The study of neutrino oscillations is an active Ąeld of research. During the last couple of decades many experiments have measured the efects of oscillations, pushing the Ąeld from the discovery stage towards an era of precision and deeper understanding of the phe- nomenon. The IceCube Neutrino Observatory, with its low energy subarray, DeepCore, has the possibility of contributing to this Ąeld. IceCube is a 1 km3 ice Cherenkov neutrino telescope buried deep in the Antarctic glacier. DeepCore, a region of denser instrumentation in the lower center of IceCube, permits the detection of neutrinos with energies as low as 10 GeV. Every year, thousands of atmospheric neutrinos around these energies leave a strong signature in DeepCore. Due to their energy and the distance they travel before being detected, these neutrinos can be used to measure the phenomenon of oscillations. This work starts with a study of the potential of IceCube DeepCore to measure neutrino oscillations in diferent channels, from which the disappearance of νµ is chosen to move forward.
    [Show full text]
  • Results from the OPERA Experiment in the CNGS Beam
    universe Review Results from the OPERA Experiment in the CNGS Beam Alessandro Paoloni on Behalf of OPERA Collaboration † INFN—Istituto Nazionale di Fisica Nucleare—Laboratori Nazionali di Frascati, I-00044 Frascati (RM), Italy; [email protected] † The OPERA collaboration author list: Agafonova, N.; Alexandrov, A.; Anokhina, A.; Aoki, S.; Ariga, A.; Ariga, T.; Bertolin, A.; Bozza, C.; Brugnera, R.; Buonaura, A.; Buontempo, S.; Chernyavskiy, M.; Chukanov, A.; Consiglio, L.; D’Ambrosio, N.; De Lellis, G.; De Serio, M.; Del Amo Sanchez, P.; Di Crescenzo, A.; Di Ferdinando, D.; Di Marco, N.; Dmitrievsky, S.; Dracos, M.; Duchesneau, D.; Dusini, S.; Dzhatdoev, T.; Ebert, J.; Ereditato, A.; Fini, R. A.; Fornari, F.; Fukuda, T.; Galati, G.; Garfagnini, A.; Gentile, V.; Goldberg, J.; Gorbunov, S.; Gornushkin, Y.; Grella, G.; Guler, A. M.; Gustavino, C.; Hagner, C.; Hara, T.; Hayakawa, T.; Hollnagel, A.; Ishiguro, K.; Iuliano, A.; Jakovˇci´c,K.; Jollet, C.; Kamiscioglu, C.; Kamiscioglu, M.; Kim, S. H.; Kitagawa, N.; Kliˇcek,B.; Kodama, K.; Komatsu, M.; Kose, U.; Kreslo, I.; Laudisio, F.; Lauria, A.; Ljubiˇci´c,A.; Longhin, A.; Loverre, P.F.; Malgin, A.; Mandrioli, G.; Matsuo, T.; Matveev, V.; Mauri, N.; Medinaceli, E.; Meregaglia, A.; Mikado, S.; Miyanishi, M.; Mizutani, F.; Monacelli, P.; Montesi, M. C.; Morishima, K.; Muciaccia, M. T.; Naganawa, N.; Naka, T.; Nakamura, M.; Nakano, T.; Niwa, K.; Ogawa, S.; Okateva, N.; Ozaki, K.; Paparella, L.; Park, B. D.; Pasqualini, L.; Pastore, A.; Patrizii, L.; Pessard, H.; Podgrudkov, D.; Polukhina, N.; Pozzato, M.; Pupilli, F.; Roda, M.; Roganova, T.; Rokujo, H.; Rosa, G.; Ryazhskaya, O.; Sato, O.; Schembri, A.; Shakiryanova, I.; Shchedrina, T.; Shibayama, E.; Shibuya, H.; Shiraishi, T.; Simone, S.; Sirignano, C.; Sirri, G.; Sotnikov, A.; Spinetti, M.; Stanco, L.; Starkov, N.; Stellacci, S.
    [Show full text]
  • Measurement of the Tau Neutrino Cross Section in Atmospheric Neutrino Oscillations with Super-Kamiokande
    PHYSICAL REVIEW D 98, 052006 (2018) Measurement of the tau neutrino cross section in atmospheric neutrino oscillations with Super-Kamiokande Z. Li,9 K. Abe,1,37 C. Bronner,1 Y. Hayato,1,37 M. Ikeda,1 K. Iyogi,1 J. Kameda,1,37 Y. Kato,1 Y. Kishimoto,1,37 Ll. Marti,1 M. Miura,1,37 S. Moriyama,1,37 M. Nakahata,1,37 Y. Nakajima,1,37 Y. Nakano,1 S. Nakayama,1,37 A. Orii,1 G. Pronost,1 H. Sekiya,1,37 M. Shiozawa,1,37 Y. Sonoda,1 A. Takeda,1,37 A. Takenaka,1 H. Tanaka,1 S. Tasaka,1 T. Tomura,1,37 R. Akutsu,2 T. Kajita,2,37 Y. Nishimura,2 K. Okumura,2,37 K. M. Tsui,2 P. Fernandez,3 L. Labarga,3 F. d. M. Blaszczyk,4 J. Gustafson,4 C. Kachulis,4 E. Kearns,4,37 J. L. Raaf,4 J. L. Stone,4,37 L. R. Sulak,4 S. Berkman,5 S. Tobayama,5 M. Elnimr,6 W. R. Kropp,6 S. Locke,6 S. Mine,6 P. Weatherly,6 M. B. Smy,6,37 H. W. Sobel,6,37 V. Takhistov,6,* K. S. Ganezer,7 J. Hill,7 J. Y. Kim,8 I. T. Lim,8 R. G. Park,8 A. Himmel,9 E. O’Sullivan,9 K. Scholberg,9,37 C. W. Walter,9,37 T. Ishizuka,10 T. Nakamura,11 J. S. Jang,12 K. Choi,13 J. G. Learned,13 S. Matsuno,13 S. N. Smith,13 J. Amey,14 R.
    [Show full text]
  • Highlight Talk from Super-Kamiokande †
    Communication Highlight Talk from Super-Kamiokande † Yuuki Nakano and on behalf of the Super-Kamiokande Collaboration Kamioka Observatory, Institute for Cosmic Ray Research, The University of Tokyo, Higashi-Mozumi 456, Kamioka-cho, Hida-city Gifu 506-1205, Japan; [email protected]; Tel.: +81-578-85-9665 † This paper is based on the talk at the 7th International Conference on New Frontiers in Physics (ICNFP 2018), Crete, Greece, 4–12 July 2018. Received: 30 November 2018; Accepted: 7 January 2019; Published: 9 January 2019 Abstract: Super-Kamiokande (SK), a 50 kton water Cherenkov detector in Japan, is observing both atmospheric and solar neutrinos. It is also searching for supernova (relic) neutrinos, proton decays and dark matter-like particles. A three-flavor oscillation analysis was conducted with the atmospheric neutrino data to study the mass hierarchy, the leptonic CP violation term, and other oscillation parameters. In addition, the observation of solar neutrinos gives precise measurements of the energy spectrum and oscillation parameters. In this proceedings, we given an overview of the latest results from SK and the prospect toward the future project of SK-Gd. Keywords: Super-Kamiokande; atmospheric neutrino; solar neutrino; neutrino oscillation; CP violation; proton decay 1. Introduction A theoretical framework of neutrino oscillation has been established in the past 50 years [1,2]. Neutrino physics has been dominated by the measurement of oscillation parameters and such measurements suggest that neutrinos are massive and mixing in the lepton sector [3]. Within the three- 2 2 flavor framework, three mixing angles (q12, q23, and q13) and two mass splittings (Dm21 and Dm32,31) are measured among neutrino experiments.
    [Show full text]