Neutrino detectors 1) Very small cross-sections of interactions → very big volumes of detectors 2) Very effective shielding → underground detectors, under pes: 1) Radiochemical detectors 2) Detectors of Cherenkov radiation 3) Scintillation detectors 4) Detectors based on neutrino scattering on electr Neutrino detector KAMLAND at Japan Underwater neutrino detector ANTARES Kamiokande
Neutrino detectors. Basic features: 1) Very small cross-sections of interactions → very big volumes of detectors 2) Very effective shielding → underground detectors, underwater, - PowerPoint PPT Presentation
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Neutrino detectors
Basic features: 1) Very small cross-sections of interactions → very big volumes of detectors 2) Very effective shielding → underground detectors, underwater, under ice
Detector types: 1) Radiochemical detectors
2) Detectors of Cherenkov radiation
3) Scintillation detectors
4) Detectors based on neutrino scattering on electrons
Neutrino detector KAMLAND at Japan Underwater neutrino detectorANTARESKamiokande
Radiochemical detectors
For example: νe + 37Cl → 37Ar + e-
νe + 71Ga → 71Ge + e-
For neutrinos with lower energy. Inverse beta decay process:
Scheme of gallium experiment – separation of produced germanium
Chlorine experiment of R. Davise
Impossibility of neutrino energydetermination (only threshold)
Measurement cycle: 1) Taking of data 2) Radiochemical analysis
Detectors making use of scintillation or Cherenkov radiation
Vessel: 1) Walls are covered by photomultipliers 2) Filled by liquid (liquid scintillator)
Scintillation detector LSND Kamoikande detector – Cherenkov phenomenais used
Detector KAMLAND
Heavy water – reaction of neutrinos with deuteron:
Photomultiplier of KAMLAND detectorDetector KAMLAND
Reaction of all neutrinos and antineutrinos:Reaction of only electronneutrinos:
(liquid scintillator)
IceCube (AMANDA) – neutrino detector under ice
200 TeV e candidate
Detector set-up built up on South pole
Photomultipliers are sentunder ice
Detection of Cherenkov radiation produced by electrons, muons and tauons produced by reactions of high energy neutrinos
Neutrino scattering on electron
Possibility to detect also neutrinos with very low energy
Noise suppression → liquid helium (superfluid) → very low temperature (~ 10 mK)
Microcalorimetry of very small temperature changes
Low neutrino energy ~ keV → low electron energy
Ionization, scintillation, phonons, rotons – are detected by sapphire or silicon wafer – absorber → control of temperature
capture of „drifting electrons – „electron bubble“ in superfluid and superconductive liquid moves in controlledway in electric field