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Pourquoi l’étude des neutrinos !?! 31 ième Congrès de la FAAQ 2006: • Plaisir – Curiosité – Passion • Science d’observation • Physique et astronomie Le neutrino: • La particule la plus abondante dans l’univers après le photon • Nos origines et la fabrique de l’espace/temps • Mieux comprendre la matière et les lois fondamentales qui gouvernent le cosmos L’Observatoire de Neutrinos de Sudbury: • Étoiles… sources de neutrinos • Étude de notre soleil • Implication en physique subatomique FAAQ2006 Alain Bellerive 2 F U N S C I E N C E !
Les grandes questions du 21 ième siècle en astrophysique des particules • Comment les particules acquièrent-elles leur masse ? • Qu’est-ce que la masse manquante de l’univers ? • Pourquoi la matière domine-t-elle l’antimatière ? • Comment la matière a-t-elle évolué juste après le big bang ? FAAQ2006 Alain Bellerive 3
Page 1: Le neutrino, particule fantomatique
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 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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