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Gallium Experiments 71 Ga + ν e → 71 Ge + e - Radiochemical Target Small proportional counters are used to count the Germanium Energy Threshold: 0.233 MeV Sensitive to pp, 7 Be, 8 B, CNO, and pep ν’s SAGE: Russian-American Gallium solar neutrino Experiment (INR RAS) ‣ A liquid metal target which contains 50 tons of gallium. GALLEX/GNO: Gallium Neutrino Observatory in Gran Sasso ‣ 30 tons of natural gallium in an aqueous acid solution. FAAQ2006 Alain Bellerive 30
Gallium Measurements: SAGE (on-going) SAGE overall 1990-2003 (121 runs) 66.9 ±3.9 (stat) ±3.6 (syst) SNU Expected rate [1σ from BP2004] +12 131 SNU –10 Source: Neutrino 2004 FAAQ2006 Alain Bellerive 31
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 and 10: History of the Neutrino • Disover
Page 11 and 12: Elementary Particles electron & neu
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: Chlorine Measurements: Homestake (U
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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