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

3 6 9

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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