1. Particle Physics: Status and Perspectives Part 7: Neutrinos Manfred Jeitler

2. 2

3. 3 neutrino oscillations  old idea: in analogy to K 0 -    oscillations, neutrinos might also change their flavor  “mass eigenstates” would not be “Weak eigenstates”  first put forward by Bruno Pontecorvo (1957, 1967)  “solar neutrino deficit”: too few ν e observed from sun  theory seemed convincing because of known solar energy  basic process is  p + p  d + e + + ν  over long time, only one experiment (“Homestead mine”, Ray Davies)

4. 4 The Homestake gold mine (South Dakota, USA) 1889 today

5. 5 The Homestake solar neutrino detector (1500 m under ground)

6. 6 Raymond Davis Nobel prize 2002

7. 7

8. 8

9. 9 neutrino oscillations

10. 10 neutrino oscillations

11. 11 neutrino mixing  both electron-neutrinos and muon-neutrinos mix  solar neutrino deficit: too few ν e from sun  atmospheric neutrino deficit: too few ν μ from atmosphere  cosmic radiation creates pions  π +/-  μ +/- ν e  strong mixing  much stronger than in quark sector  low masses  Δm 2 solar  10 -4 eV 2  Δm 2 atmos  2  10 -3 eV 2  we know only mass differences, not masses themselves  origin of neutrino mass?  beyond Standard Model!  “see-saw” mechanism?

12. 12 the Superkamiokande neutrino detector (Japan)

13. 13 atmospheric neutrinos

14. 14

15. 15

16. 16

17. 17 Long-baseline experiments

18. Messengers from the Universe  Photons currently provide all information on the Universe. But they are rather strongly reprocessed and absorbed in their sources and during propagation. For E g > 500 TeV photons do not survive journey from Galactic Centre.  Protons+Nuclei: directions scrambled by galactic and intergalactic magnetic fields. Also, for E pr >20 21 eV they lose energy due to interaction with relict radiation (GZK-effect: Greisen-Zatsepin- Kuzmin limit).  Neutrinos have discovery potential because they open a new window onto the universe W49B SN 0540-69.3 Crab E0102-72.3 Cas A  P+Nuclei

19. 1960 - M. Markov: High Energy neutrino detection in natural transparent media (ocean water, ice): O(km) long muon tracks  5-15 m Charged Current (CC)  Electromagnetic & hadronic cascades ~ 5 m CC e  + Neutral Current

20. log(E 2  Flux) log(E/GeV) TeV PeV EeV 3 6 9 pp core AGN p  blazar jet GZK GRB (W&B) WIMPs WIMPsOscillations Underground Underwater Radio,Acoustic Air showers Microquasars etc.

21. A NT200+/Baikal-GVD 1993-1998 (~2015) N N KM3NeT (~2014) /IceCube Amanda/IceCube (now) 1996-2000 (now) ANTARES NEMO NESTOR

26. Schematic view on the deep underwater complex NT200 10-Neutrino Telescope NT200 7-hydrophysical mooring 5-sedimentology mooring 12-geophysical mooring 13-18-acoustic transponders 1-4 cable lines Anchor Buoy

27. NT200 running since 1998 - - 8 strings with 192 optical modules, - 72m height, - R=21.5m radius, -1070m depth, Vgeo=0.1Mton  effective area: S >2000 m 2 (E  >1 TeV) Shower Eff Volume: ~1 Mt at 1 PeV

30. ICECUBE 30

31. 31

32. 32