particle physics: status and perspectives part 7: neutrinos manfred jeitler
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Particle Physics: Status and PerspectivesPart 7: Neutrinos
Manfred Jeitler
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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)
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The Homestake gold mine (South Dakota,
USA)
1889 today
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The Homestake solar neutrino detector(1500 m under ground)
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Raymond Davis
Nobel prize 2002
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neutrino oscillations
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neutrino oscillations
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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 Δm2
solar 10-4 eV2
Δm2atmos 210-3 eV2
we know only mass differences, not masses themselves origin of neutrino mass?
beyond Standard Model! “see-saw” mechanism?
12the Superkamiokande neutrino detector (Japan)
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atmospheric neutrinos
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Long-baseline experiments
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).
NeutrinosNeutrinos have discovery potential because they have discovery potential because they open a new window onto the universeopen a new window onto the universe
W49B
SN 0540-69.3
Crab
E0102-72.3
Cas A
P+Nuclei
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
log(
E2
Flu
x)
log(E/GeV)TeV PeV EeV
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pp core AGN p blazar jet
GZK
GRB (W&B)
WIMPsWIMPsOscillationsOscillations
UndergroundUnderground
UnderwaterUnderwaterRadio,AcousticRadio,Acoustic
Air showersAir showers
Microquasars etc.
A
NT200+/Baikal-GVD1993-1998 (~2015)
N N
KM3NeT(~2014)
Amanda/IceCube/IceCube1996-2000 (now)(now)
ANTARES
NEMO
NESTOR
Schematic view on the deep underwater complex NT200
10-Neutrino Telescope NT2007-hydrophysical mooring 5-sedimentology mooring
12-geophysical mooring 13-18-acoustic transponders 1-4 cable lines
Anchor
Buoy
NANPNANP’’0303
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 m2 (E>1 TeV)Shower Eff Volume: ~1 Mt at 1 PeV
ICECUBE
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