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Reactor & Accelerator 

Reactor & Accelerator . Thanks to Bob McKeown for many of the slides. Outline. Reactor Neutrinos The neutrinos Past experiments What we know and what we want to learn Accelerator Neutrinos The neutrinos Past experiments What we know and what we want to learn. n e Disappearance.

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Reactor & Accelerator 

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  1. Reactor & Accelerator  Thanks to Bob McKeown for many of the slides

  2. Outline • Reactor Neutrinos The neutrinos Past experiments What we know and what we want to learn • Accelerator Neutrinos The neutrinos Past experiments What we know and what we want to learn Steve Elliott, NPSS 2005

  3. neDisappearance Dominant 12Oscillation P(ee) Distance (m) Subdominant 13Oscillation Steve Elliott, NPSS 2005

  4. Solar q13 hep-ph/0309130 90, 95, 99% CL Chooz m232 from SK atmospheric Steve Elliott, NPSS 2005

  5. Neutrino Oscillation Studies with Nuclear Reactors • ne from n-rich fission products • detection via inverse beta decay (ne+pge++n) • Measure flux and energy spectrum • Improve detectors, reduce background • Variety of distances L= 10m-250km Steve Elliott, NPSS 2005

  6. g 2.2 MeV d + p e n n g g 511keV 511keV Detection Signal Coincidence signal: detect • Prompt: e+ annihilation g En=Eprompt+En+0.8 MeV • Delayed: n capture 180 ms capture time Steve Elliott, NPSS 2005

  7. Steve Elliott, NPSS 2005

  8. Kashiwazaki Takahama Ohi KamLAND uses the entire Japanese nuclear power industry as a long­baseline source Steve Elliott, NPSS 2005

  9. Steve Elliott, NPSS 2005

  10. Ratio of Measured and Expected e Flux from Reactor Neutrino Experiments Solar n: Dm2 = 5.5x10-5 eV2 sin2 2Q = 0.833 G.Fogli et al., PR D66, 010001-406, (2002) Steve Elliott, NPSS 2005

  11. Measurement of Energy Spectrum Steve Elliott, NPSS 2005

  12. KamLAND best fit : Dm2 = 7.9 x 10-5 eV2 tan2q = 0.45 KamLAND fixes mass Solar fixes angle Steve Elliott, NPSS 2005

  13. New Reactor Proposals Daya Bay, China • ~1.5 km baseline • Deeper/bigger • Near/Far Braidwood, Il Chooz, France Steve Elliott, NPSS 2005

  14. horizontal cylinder Detector Design Studies horizontal cylinder spherical Steve Elliott, NPSS 2005

  15. Oscillation Formulae for Long-Baseline Neutrinos For anti-neutrinos, the Jcp terms change sign. Steve Elliott, NPSS 2005

  16. Long Baseline Physics Goals • Definitive observation of oscillatory behavior in  disappearance mode and precise determination of m223 and 23. • Detection of oscillation e in appearance mode and measurement of 13. • Observe matter effects, hence sign of m223. • Measure cp Steve Elliott, NPSS 2005

  17. CP violation and matter effects hep-ph/0306221 Steve Elliott, NPSS 2005

  18. T2K Phase I 0.75 MW +SK Phase II 4 MW + HyperK Steve Elliott, NPSS 2005

  19. HyperK Steve Elliott, NPSS 2005

  20. NOA Use the NUMI beam line from FermiLab. Far detector uses alternate vertical planes of active scintillator with passive wood absorber. Steve Elliott, NPSS 2005

  21. Off-Axis Beam • For pions decaying in flight, most neutrinos are forward directed • Neutrino energy is proportional to E • Neutrino energy flattens with angle, however. Allowing one to “choose” an energy by choosing the angle. Steve Elliott, NPSS 2005

  22. Far Detector 810 km from target 10-14 km off axis Steve Elliott, NPSS 2005

  23. LONG baseline 2500-3000 km Steve Elliott, NPSS 2005

  24. The LSND Puzzle and MiniBOONE Steve Elliott, NPSS 2005

  25. The Evidence for Neutrino Oscillations Steve Elliott, NPSS 2005

  26. Requires a 3rdm2 Steve Elliott, NPSS 2005

  27. Steve Elliott, NPSS 2005

  28. Steve Elliott, NPSS 2005

  29. Measurement of Oscillation Parameters Steve Elliott, NPSS 2005

  30. Typical Muon-Neutrino Event Steve Elliott, NPSS 2005

  31. Typical Michel Electron Event Steve Elliott, NPSS 2005

  32. Resources • Bob Mckeown APS April 2005 (Tampa) • APS neutrino study on reactors and long baseline experiments. • BNL, T2K and NOA Letters of Intent • Bill Louis Talks Steve Elliott, NPSS 2005

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