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Particle Physics: Status and Perspectives Part 7: Neutrinos Manfred Jeitler
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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)
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4 The Homestake gold mine (South Dakota, USA) 1889 today
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5 The Homestake solar neutrino detector (1500 m under ground)
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6 Raymond Davis Nobel prize 2002
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9 neutrino oscillations
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10 neutrino oscillations
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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?
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12 the Superkamiokande neutrino detector (Japan)
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13 atmospheric neutrinos
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17 Long-baseline experiments
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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
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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
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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.
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A NT200+/Baikal-GVD 1993-1998 (~2015) N N KM3NeT (~2014) /IceCube Amanda/IceCube (now) 1996-2000 (now) ANTARES NEMO NESTOR
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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
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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
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ICECUBE 30
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