1. Solar & Atmospheric

2. June 2005Steve Elliott, NPSS 20052 Outline Neutrinos from the Sun The neutrinos Past experiments What we know and what we want to learn Atmospheric Neutrinos The neutrinos Past experiments What we know and what we want to learn

3. June 2005Steve Elliott, NPSS 20053 Solar Model Assumptions Hydrostatic Equilibrium –radiative & particle pressures balance gravity Energy Transport –photon diffusion in deep interior Energy Generation –nuclear fusion Isotopic/Elemental Abundances –changes occur only by nuclear reactions –initially agrees with current surface observations

4. June 2005Steve Elliott, NPSS 20054 The pp fusion reactions p + e - + p  2 H + e 2 H + p  3 He +  3 He + p  4 He + e + + e 3 He + 4 He  7 Be +  7 Be + e -  7 Li +  + e 7 Li + p   +  3 He + 3 He  4 He + 2p 99.75%0.25% 85%~15% 0.02%15.07% ~10 -5 % 7 Be + p  8 B +  8 B  8 Be* + e + + e p + p  2 H + e + + e

5. June 2005Steve Elliott, NPSS 20055 The energy spectrum

6. June 2005Steve Elliott, NPSS 20056 MSW at high energies, vacuum at low. Ratio of oscillation length in matter to vacuum

7. June 2005Steve Elliott, NPSS 20057 Matter and Vacuum matter vacuum About 1 MeV For the Sun If  < cos2  12 ~0.4 then the oscillation probability is given by the vacuum averaged result. hep-ph/0305159

8. June 2005Steve Elliott, NPSS 20058 The Cl Experiment Ray Davis and his tank of cleaning fluid

9. June 2005Steve Elliott, NPSS 20059 Cl Operations 615 tons of C 2 Cl 4, 814-keV threshold Homestake Gold Mine Bubble He gas through to extract Ar Ar trapped in cold trap. PC filled with Ar gas (7% methane) 37 Cl is 24% abundant.

10. June 2005Steve Elliott, NPSS 200510 The Homestake Mine

11. June 2005Steve Elliott, NPSS 200511 The Cl Apparatus

12. June 2005Steve Elliott, NPSS 200512 Cl Results 2.56 ± 0.16 ± 0.16 SNU Expect 7.5 SNU

13. June 2005Steve Elliott, NPSS 200513 SAGE and Gallex (GNO) 71 Ga( e,e) 71 Ge 71 Ge has 11.4 day half life. Expose Ga to neutrinos Extract Ge and count via its decay.

14. June 2005Steve Elliott, NPSS 200514 SAGE Operations 1.Add carrier to Ga. 2.After about 3-4 weeks, extract Ge carrier and solar neutrino induced Ge. 3.Synthesize counter gas and fill proportional counter. 4.Count sample for about 6 months.

15. June 2005Steve Elliott, NPSS 200515 Map to SAGE

16. June 2005Steve Elliott, NPSS 200516 Baksan Valley, UG Laboratory

17. June 2005Steve Elliott, NPSS 200517 Reactor Layout 10 reactors Each can hold 8 tons of Ga Kept warm so Ga is liquid

18. June 2005Steve Elliott, NPSS 200518 Results - Solar Rate Expect 128 SNU Each run saw about 6 signal Events.

19. June 2005Steve Elliott, NPSS 200519 Gran Sasso Italy: Not too far from Rome

20. June 2005Steve Elliott, NPSS 200520 GNO Layout

21. June 2005Steve Elliott, NPSS 200521 GALLEX Results Expected 128 SNU

22. June 2005Steve Elliott, NPSS 200522 Kamiokande & SuperK Elastic scattering of e - in a large water detector Mostly sensitive to e because CC cross section is about 6x higher than NC

23. June 2005Steve Elliott, NPSS 200523 SNO ES, CC, and NC CC: d( e, pp)e - –Sensitive only to e NC: d( x, np) x –Sensitive to all x NC/CC ratio

24. June 2005Steve Elliott, NPSS 200524 SNO data Radius of event vertex Angle with Sun

25. June 2005Steve Elliott, NPSS 200525 Event Energy

26. June 2005Steve Elliott, NPSS 200526 NC vs. CC response

27. June 2005Steve Elliott, NPSS 200527 The hierarchy question Normal Inverted

28. June 2005Steve Elliott, NPSS 200528 The “Dark Side” of solar neutrinos Two “flavors” are involved in solar neutrino oscillations. e and a linear combination of   and .

29. June 2005Steve Elliott, NPSS 200529 The “Dark Side” of solar neutrinos II For  <  /4, 1 is mostly e. But for  ’ =  /2 -  /4, 1 is mostly  + . Thus, although oscillations in a vacuum cannot distinguish between  and  ’, matter oscillations can. That is cos2  changes sign.

30. June 2005Steve Elliott, NPSS 200530 Solar Neutrino Results there is no dark side Early fit to solar neutrino data. Note solution space for tan  >1. Phys.Lett. B490 (2000) 125

31. June 2005Steve Elliott, NPSS 200531 The addition of KamLAND

32. June 2005Steve Elliott, NPSS 200532 What’s left to do? Is our model of neutrino mixing and oscillation complete, or are there other mechanisms at work? –Without luminosity constraint, pp and 7 Be fluxes poorly known. –With constraint, 7 Be is still poorly known. Is nuclear fusion the only source of the Sun’s energy and is it steady state? What is the correct hierarchial ordering of the neutrino masses?

33. June 2005Steve Elliott, NPSS 200533 Non-Standard transformation possibilities Violation of equivalence principle Violation of Lorentz principle Non universal coupling Violation of Lorentz invariance due to CPT violating terms Non-standard neutrino interactions

34. June 2005Steve Elliott, NPSS 200534 Future Solar Neutrino Experiments ExperimentTargetReactionThreshold Borexino ~300 t liq. Scint. ES~250 keV KamLAN D ~600 t liq scint. ES~250 keV LENS 60 t In load in scint CC HERON68 m 3 LHeES~45 keV CLEAN40 t liq. NeES~35 keV MOON Few t of 100 Mo CC168 keV

35. June 2005Steve Elliott, NPSS 200535 Atmospheric Neutrinos Up vs. Down

36. June 2005Steve Elliott, NPSS 200536 IMB and Kamiokande Previous large water Cherenkov detectors Built to look for proton decay, atmospheric neutrinos are a significant background: hence lots of study Kamiokande was able to lower threshold to see solar neutrinos Saw SN1987A, but not pdk Statistically weak indication of atmospheric neutrino oscillations Led to plan for Very Large SuperK

37. June 2005Steve Elliott, NPSS 200537 SuperK 1000 m underground 50,000 tons of water 12,000 pmts

38. June 2005Steve Elliott, NPSS 200538 Results

39. June 2005Steve Elliott, NPSS 200539 Maximal mixing and the future If sin 2  13 is different than 0, Earth matter effects can resonantly enhance the subdominate transitions depending on the sign of  m 23 2.

40. June 2005Steve Elliott, NPSS 200540 Future Experiments ExperimentTargetStatus SuperK50 kt waterContinue on SNO1 kt heavy water Continue on MINOS Iron magnetized calorimeter Operating, but small INO 30-50kt magnetized tracking calorimeter proposal UNO/HyperK Mt class waterproposal

41. June 2005Steve Elliott, NPSS 200541 SNO is “small” but deep

42. June 2005Steve Elliott, NPSS 200542 Resources Andrew Hime colloquium APS neutrino study on solar and atmospheric neutrinos