48 pp.
48 pp.
| 1352 K 48 pp. | |
| View Document | ||
| Title | Status and Aims of the DUMAND Neutrino Project: the Ocean as a Neutrino Detector | |
| Author(s) | Roberts, A.; Blood, H.; Learned, J.; Reines, F. | |
| Publication Date | July 1976 | |
| Report Number | FERMILAB-Conf-76/59-EXP | |
| Unique Identifier | ACC0159 | |
| Other Numbers | CONF-760671-9; OSTI ID: 7332526 | |
| Research Org | Fermi National Accelerator Laboratory, Batavia, Ill. (USA) [FNAL] | |
| Contract No | E(49-8)-3000 | |
| Sponsoring Org | Energy Research and Development Administration (ERDA) | |
| Other Information | International Neutrino Conference; 8 June 1976; Aachen, F.R. Germany | |
| Subject | 440104 -- Radiation Instrumentation -- High Energy Physics Instrumentation; 640106 -- Astrophysics & Cosmology -- Cosmology; 645102 -- High Energy Physics -- Particle Interactions & Properties - Experimental -- Weak Interactions & Properties; Cherenkov Counters -- Feasibility Studies; Neutrino Detection -- Cherenkov Counters; Cherenkov Radiation; Cosmic Showers; Gravitational Collapse; Seawater; Underwater | |
| Keywords | Cosmic Radiation; Electromagnetic Radiation; Hydrogen Compounds; Ionizing Radiations; Levels; Measuring Instruments; Oxygen Compounds; Radiation Detection; Radiation Detectors; Radiations; Secondary Cosmic Radiation; Showers; Water | |
| Related Web Pages | Frederick Reines and the Detection of the Neutrino | |
| Abstract | The possibility of using the ocean as a neutrino detector is considered. Neutrino-produced interactions result in charged particles that generate Cherenkov radiation in the water, which can be detected by light-gathering equipment and photomultipliers. The properties of the ocean as seen from this standpoint are critically examined, and the advantages and disadvantages pointed out. Possible uses for such a neutrino detector include (1) the detection of neutrinos emitted in gravitational collapse of stars (supernova production), not only in our own galaxy, but in other galaxies up to perhaps twenty-million light-years away, (2) the extension of high-energy neutrino physics, as currently practiced up to 200 GeV at high-energy accelerators, to energies up to 50 times higher, using neutrinos generated in the atmosphere by cosmic rays, and (3) the possible detection of neutrinos produced by cosmic-ray interactions outside the earth`s atmosphere. The technology for such an undertaking seems to be within reach. | |
| 1352 K 48 pp. | |
| View Document | ||
