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

3. June 2005Steve Elliott, NPSS 20052 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

4. June 2005Steve Elliott, NPSS 20053 Distance (m) P( e  e ) Dominant  12 Oscillation Subdominant  13 Oscillation e Disappearance

5. June 2005Steve Elliott, NPSS 20054  13 90, 95, 99% CL hep-ph/0309130  m 23 2 from SK atmospheric Chooz Solar

6. June 2005Steve Elliott, NPSS 20055 Neutrino Oscillation Studies with Nuclear Reactors e from n-rich fission products detection via inverse beta decay ( e +p  e + +n) Measure flux and energy spectrum Improve detectors, reduce background Variety of distances L= 10m-250km

7. June 2005Steve Elliott, NPSS 20056 Detection Signal Coincidence signal: detect Prompt: e + annihilation  E  E prompt +E n +0.8 MeV Delayed: n capture 180  s capture time p + e 511keV   2.2 MeV  d n

8. June 2005Steve Elliott, NPSS 20057

9. June 2005Steve Elliott, NPSS 20058 KamLAND uses the entire Japanese nuclear power industry as a long­baseline source Kashiwazaki Takahama Ohi

10. June 2005Steve Elliott, NPSS 20059

11. June 2005Steve Elliott, NPSS 200510 Solar :  m 2 = 5.5x10 -5 eV 2 sin 2 2  = 0.833 G.Fogli et al., PR D66, 010001-406, (2002) Ratio of Measured and Expected e Flux from Reactor Neutrino Experiments

12. June 2005Steve Elliott, NPSS 200511 Measurement of Energy Spectrum

13. June 2005Steve Elliott, NPSS 200512 KamLAND best fit :  m 2 = 7.9 x 10 -5 eV 2 tan 2  = 0.45 KamLAND fixes mass Solar fixes angle

14. June 2005Steve Elliott, NPSS 200513 New Reactor Proposals Braidwood, Il Daya Bay, China Chooz, France ~1.5 km baseline Deeper/bigger Near/Far

15. June 2005Steve Elliott, NPSS 200514 Detector Design Studies horizontal cylinder spherical

16. June 2005Steve Elliott, NPSS 200515 Oscillation Formulae for Long- Baseline Neutrinos For anti-neutrinos, the J cp terms change sign.

17. June 2005Steve Elliott, NPSS 200516 Long Baseline Physics Goals Definitive observation of oscillatory behavior in   disappearance mode and precise determination of  m 2 23 and  23. Detection of oscillation   e in appearance mode and measurement of  13. Observe matter effects, hence sign of  m 2 23. Measure  cp

18. June 2005Steve Elliott, NPSS 200517 CP violation and matter effects hep-ph/0306221

19. June 2005Steve Elliott, NPSS 200518 T2K Phase I 0.75 MW +SK Phase II 4 MW + HyperK

20. June 2005Steve Elliott, NPSS 200519 HyperK

21. June 2005Steve Elliott, NPSS 200520 NO A Use the NUMI beam line from FermiLab. Far detector uses alternate vertical planes of active scintillator with passive wood absorber.

22. June 2005Steve Elliott, NPSS 200521 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.

23. June 2005Steve Elliott, NPSS 200522 Far Detector 810 km from target 10-14 km off axis

24. June 2005Steve Elliott, NPSS 200523 LONG baseline 2500-3000 km

25. June 2005Steve Elliott, NPSS 200524 The LSND Puzzle and MiniBOONE

26. June 2005Steve Elliott, NPSS 200525 The Evidence for Neutrino Oscillations

27. June 2005Steve Elliott, NPSS 200526 Requires a 3 rd  m 2

28. June 2005Steve Elliott, NPSS 200527

29. June 2005Steve Elliott, NPSS 200528

30. June 2005Steve Elliott, NPSS 200529 Measurement of Oscillation Parameters

31. June 2005Steve Elliott, NPSS 200530 Typical Muon-Neutrino Event

32. June 2005Steve Elliott, NPSS 200531 Typical Michel Electron Event

33. June 2005Steve Elliott, NPSS 200532 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