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  2. Cherenkov detector - Wikipedia

    en.wikipedia.org/wiki/Cherenkov_detector

    Cherenkov threshold detectors have been used for fast timing and time of flight measurements in particle detectors. More elaborate designs use the amount of light produced. Recording light from both primary and secondary particles, for a Cherenkov calorimeter the total light yield is proportional to the incident particle energy.

  3. Neutrino detector - Wikipedia

    en.wikipedia.org/wiki/Neutrino_detector

    In a Cherenkov detector, a large volume of clear material such as water or ice is surrounded by light-sensitive photomultiplier tubes. A charged lepton produced with sufficient energy and moving through such a detector does travel somewhat faster than the speed of light in the detector medium (although somewhat slower than the speed of light in ...

  4. Accelerator Neutrino Neutron Interaction Experiment - Wikipedia

    en.wikipedia.org/wiki/Accelerator_Neutrino...

    The Accelerator Neutrino Neutron Interaction Experiment (ANNIE) is a water Cherenkov detector experiment designed to examine the nature of neutrino interactions. This experiment studies phenomena like proton decay, and neutrino oscillations, by analyzing neutrino interactions in gadolinium-loaded water and measuring their neutron yield.

  5. Cosmic-ray observatory - Wikipedia

    en.wikipedia.org/wiki/Cosmic-ray_observatory

    KASCADE-(Grande) – KArlsruhe Shower Core and Array DEtector (and its extension called 'Grande') Large High Altitude Air Shower Observatory; LOPES – the LOFAR PrototypE Station is the radio extension of KASCADE. TAIGA – Tunka Advanced Instrument for cosmic ray physics and Gamma Astronomy; HAWC High Altitude Water Cherenkov

  6. Chicago Air Shower Array - Wikipedia

    en.wikipedia.org/wiki/Chicago_Air_Shower_Array

    The CASA scintillation detectors are the white square boxes laid out on a 15-meter grid spacing. At the center of the array (left of center in this image) is the Fly's Eye II detector. Prior to CASA, air shower arrays were typically modest in size, typically consisting of 50-100 detectors covering an area of around 50,000 square meters.

  7. Pierre Auger Observatory - Wikipedia

    en.wikipedia.org/wiki/Pierre_Auger_Observatory

    Surface detector (SD) station, or 'tank', of the Pierre Auger Observatory. In 1967 University of Leeds had developed a water-Cherenkov detector (or surface station; a small water basin, 1.2 m deep; also called tank) and created a 12 km 2 detection area Haverah Park using 200 such tanks. They were arranged in groups of four in a triangular (Y ...

  8. NEVOD - Wikipedia

    en.wikipedia.org/wiki/NEVOD

    NEVOD (Russian: НЕВОД, НЕйтринный ВОдный Детектор, Neutrino Water Detector; nevod means "dragnet" in Russian) is a neutrino detector and cosmic ray experiment that attempts to detect Cherenkov radiation arising from interactions between water and charged particles (mostly muons). It represents the first attempt to ...

  9. Haverah Park experiment - Wikipedia

    en.wikipedia.org/wiki/Haverah_Park_experiment

    The Haverah Park experiment was a cosmic ray air shower detection array consisting of water Cherenkov detectors [1] distributed over an area of 12 km 2 on Haverah Park on the Pennine moorland near Harrogate, North Yorkshire. The experiment was operated by University of Leeds for 20 years, and was switched off in 1987.