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Particle Physics: Status and Perspectives Part 7: Neutrinos

Particle Physics: Status and Perspectives Part 7: Neutrinos. SS 2014. Manfred Jeitler. neutrino oscillations. old idea: in analogy to K 0 -    oscillations, neutrinos might also change their flavor “mass eigenstates” would not be “Weak eigenstates”

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Particle Physics: Status and Perspectives Part 7: Neutrinos

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  1. Particle Physics: Status and PerspectivesPart 7: Neutrinos SS 2014 Manfred Jeitler

  2. neutrino oscillations • old idea: in analogy to K0 - 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 νe 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)

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

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

  5. Raymond Davis Nobel prize 2002

  6. neutrino oscillations

  7. neutrino oscillations

  8. neutrino mixing both electron-neutrinos and muon-neutrinos mix solar neutrino deficit: too few νe from sun atmospheric neutrino deficit: too few νμ from atmosphere cosmic radiation creates pions π+/-  μ+/- νe strong mixing much stronger than in quark sector low masses Δm2solar 10-4 eV2 Δm2atmos 210-3 eV2 we know only mass differences, not masses themselves origin of neutrino mass? beyond Standard Model! “see-saw” mechanism?

  9. the Superkamiokande neutrino detector (Japan)

  10. atmospheric neutrinos

  11. Long-baseline experiments

  12. W49B g n SN 0540-69.3 P+Nuclei Crab Cas A E0102-72.3 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 Eg > 500 TeV photons do not survive journey from Galactic Centre. • Protons+Nuclei: directions scrambled by galactic and intergalactic magnetic fields. Also, for Epr >2021 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

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

  14. pp core AGN p blazar jet log(E2 Flux) GZK WIMPs Oscillations GRB (W&B) 3 6 9 log(E/GeV) TeV PeV EeV Air showers Underground Radio,Acoustic Underwater Microquasars etc.

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

  16. 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 Buoy Anchor

  17. NANP’03 • NT200running since 1998 • - 8 strings with 192 optical modules, • 72m height, • R=21.5m radius, • 1070m depth, Vgeo=0.1Mton • effective area: S >2000 m2 (E>1 TeV) • Shower Eff Volume: ~1 Mt at 1 PeV

  18. ICECUBE

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