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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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Presentation Transcript
neutrino oscillations
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)
slide6

Raymond Davis

Nobel prize 2002

neutrino mixing
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?

messengers from the universe

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
1960 m markov high energy neutrino detection in natural transparent media ocean water ice

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):
slide20

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.

slide21

NT200+/Baikal-GVD

1993-1998 (~2015)

KM3NeT

(~2014)

ANTARES

A

N

N

NEMO

NESTOR

Amanda/IceCube

1996-2000 (now)

schematic view on the deep underwater complex nt200
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

slide27

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