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Neutrino Physics - Lecture 5

Neutrino Physics - Lecture 5. Steve Elliott LANL Staff Member UNM Adjunct Professor 505-665-0068, elliotts@lanl.gov. Lecture 5 Outline. Finish Solar Neutrinos Neutrinos from the Atmosphere The neutrinos Past experiments What we know and what we want to learn. The hierarchy question.

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Neutrino Physics - Lecture 5

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  1. Neutrino Physics - Lecture 5 Steve Elliott LANL Staff Member UNM Adjunct Professor 505-665-0068, elliotts@lanl.gov

  2. Lecture 5 Outline • Finish Solar Neutrinos • Neutrinos from the Atmosphere The neutrinos Past experiments What we know and what we want to learn Steve Elliott, UNM Seminar Series

  3. The hierarchy question Normal Inverted Steve Elliott, UNM Seminar Series

  4. The “Dark Side” of solar neutrinos Two “flavors” are involved in solar neutrino oscillations. e and a linear combination of  and . Steve Elliott, UNM Seminar Series

  5. 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. Steve Elliott, UNM Seminar Series

  6. Solar Neutrino Resultsthere is no dark side Early fit to solar neutrino data. Note solution space for tan>1. Phys.Lett. B490 (2000) 125 Steve Elliott, UNM Seminar Series

  7. The addition of KamLAND Steve Elliott, UNM Seminar Series

  8. Steve Elliott, UNM Seminar Series

  9. 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 7Be fluxes poorly known. • With constraint, 7Be 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? Steve Elliott, UNM Seminar Series

  10. Non-Standard Interactions and New Properties • Do neutrinos have non-standard interactions? • Are there unexpected properties? • Non-standard interactions of neutrinos with matter would lead to modifications of matter effects in oscillations. • NSI on order of 10-30% of SM weak interaction are possible and compatible with accelerator and oscillation data. • Such large effects would affect solar neutrino data. Since NSI must mimic SM behavior in the matter dominated region, but be small in the vacuum region, the transition region is a good place to look. Steve Elliott, UNM Seminar Series

  11. The Vacuum-matter transition This classic LMA oscillation probability curve might be altered by NSI. About 2 MeV hep-ph/0305159 Vacuum Matter Steve Elliott, UNM Seminar Series

  12. Future Solar Neutrino Experiments Steve Elliott, UNM Seminar Series

  13. Future Experiments Steve Elliott, UNM Seminar Series

  14. Atmospheric NeutrinosUp vs. Down Steve Elliott, UNM Seminar Series

  15. 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 Steve Elliott, UNM Seminar Series

  16. SuperK • 1000 m underground • 50,000 tons of water • 12,000 pmts Steve Elliott, UNM Seminar Series

  17. Results Steve Elliott, UNM Seminar Series

  18. L/E analysis (Ishitsuka: NOON 2004) Steve Elliott, UNM Seminar Series

  19. L/E results Steve Elliott, UNM Seminar Series

  20. Maximal mixing and the future If sin213 is different than 0, Earth matter effects can resonantly enhance the subdominate transitions depending on the sign of m232. Steve Elliott, UNM Seminar Series

  21. Future Experiments Steve Elliott, UNM Seminar Series

  22. SNO is “small” but deep Steve Elliott, UNM Seminar Series

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