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History of the Neutrino • In 1931, the neutrino was postulated by the theorist Wolfgang Pauli. Pauli based his prediction on the fact that energy and momentum did not appear to be conserved in certain radioactive decays. Pauli suggested that this missing energy might be carried off by an invisible neutral particle. • Later Enrico Fermi takes the neutrino hypothesis and builds his theory of beta decay (weak interaction). • Clyde Cowan and Fred Reines announced in 1959 the discovery of a particle fitting the expected characteristics of the neutrino. This neutrino is later determined to be the partner of the electron. FAAQ2006 Alain Bellerive 10
Elementary Particles electron & neutrino proton & neutron pion (π) & kaon Carried by → Acts on → Gravity Graviton (not yet observed) All Massive Weak Electromagnetic Electroweak W + W - Z 0 Quarks and Leptons Photon Quarks and Charged Leptons and W + W - Strong Gluon Quarks and Gluons FAAQ2006 Alain Bellerive 11
Page 1 and 2: Le neutrino, particule fantomatique
Page 3 and 4: Les grandes questions du 21 ième s
Page 5 and 6: The First Piece: - Fundamental Forc
Page 7 and 8: Scope of Particle Physics FAAQ2006
Page 9: History of the Neutrino • Disover
Page 13 and 14: Open Questions in Neutrino Physics
Page 15 and 16: 2) Underground laboratories: e.g. S
Page 17 and 18: Electroweak Interactions L ( em NC)
Page 19 and 20: • Define a quark mixing matrix wh
Page 21 and 22: Evidence for Neutrino Oscillations
Page 23 and 24: Macroscopic Properties of the Sun M
Page 25 and 26: Neutrino Production in the Sun Ligh
Page 27 and 28: Solar Neutrino Experiments • Revi
Page 29 and 30: Chlorine Measurements: Homestake (U
Page 31 and 32: Gallium Measurements: SAGE (on-goin
Page 33 and 34: Water Detector: Super-Kamiokande (J
Page 35 and 36: Solar ν Flux Measurement Results C
Page 37 and 38: Solar Neutrino Problem • Historic
Page 39 and 40: Neutrino Oscillations Neutrino Stat
Page 41 and 42: Solar Neutrino Oscillations P ee =
Page 43 and 44: Matter-Enhanced Neutrino Oscillatio
Page 45 and 46: Somewhere in the Depths of Canada..
Page 47 and 48: Underground laboratory in Sudbury S
Page 49 and 50: Subury Neutrino Observatory • Tim
Page 51 and 52: Purpose of SNO • If Solar Neutrin
Page 53 and 54: Neutrino detection in SNO • PMTs
Page 55 and 56: SNO observables - event by event PM
Page 57 and 58: Neutrino Reactions in SNO CC ν e d
Page 59 and 60: An Ultraclean Environment • Highl
Page 61 and 62:
Three Ways to Catch Neutrons! (NC)
Page 63 and 64:
Subury Neutrino Observatory D 2 O R
Page 65 and 66:
Shape Constrained Neutrino Fluxes (
Page 67 and 68:
SNO NC in D 2 O (April 2002) ~ 2/3
Page 69 and 70:
Progress in 2002 on the Solar Neutr
Page 71 and 72:
Neutrino Mixing (detail) As in the
Page 73 and 74:
Subury Neutrino Observatory Salt Re
Page 75 and 76:
Charged Current (CC=ν e ) Spectrum
Page 77 and 78:
Day/Night Asymmetries A X = ( Φ (
Page 79 and 80:
SNO: Results Phase II: neutrino osc
Page 81 and 82:
NCD Deployment FAAQ2006 Alain Belle
Page 83 and 84:
What SNO might tell us in the futur
Page 85 and 86:
FAAQ2006 Alain Bellerive 85
Page 87 and 88:
Summary • SNO provided direct evi
Page 89 and 90:
Comment les particules acquièrent-
Page 91 and 92:
Qu’est-ce que la masse manquante
Page 93 and 94:
WIMP Interaction with Matter Spin i
Page 95 and 96:
Pourquoi la matière domine-t-elle
Page 97 and 98:
Conclusion • Plusieurs défis en
Page 99:
FAAQ2006 Alain Bellerive 99
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