Neutrino detector

LTD-4 Proc. 4th Int. Conf. of Low Temperature Dark Matter and Neutrino Detectors, Oxford 1991, ed. by N.E. Booth and G.L. Salmon, Editions Frontieres, Gif-sur-Yvette, France (1992)... 

Neutrino detectors are placed at great depths, at the bottom of mines and tunnels, in order to reduce interference induced by cosmic rays (Fig. 5.3). Two methods of detection have been used to date. The first is radiochemical. It involves the production by transmutation of a radioactive isotope that is easily detectable even in minute quantities. More precisely, the idea is that a certain element is transformed into another by a neutrino impact, should it occur. Inside the target nucleus, the elementary reaction is... 

Among electronic neutrino detectors is the great KAMIOKANDE experiment and its extension SUPERKAMIOKANDE. Spread out at the bottom of a mine in Japan, this device has directional sensitivity and it can thus be checked whether captured neutrinos do actually come from the Sun. 

Based upon the foregoing experiences, some researchers observed that the same reluctance to interact with matter is responsible for the neutrino s long range and ability to resist detection. Tlios, it was reasoned that an apparatus for detecting neutrinos should be massive and shielded from the interference of other particles and radiation. As a solution to these problems, some researchers proposed a deep underwater muon and neutrino detector (acronym DUMAND). 

Figure 12.18 Log-log plot of predicted neutrino fluxes from various solar nuclear reactions. The energy regions to which the neutrino detectors are sensitive are shown at the top. [From Bahcall (from Bahcall website).]...

Outline how you would construct a radiochemical neutrino detector based upon 115In. 

As shown in the previous section, light and neutral neutrinos are optimal probes for high energy astronomy, i.e. for the identification of astrophysical sources of UHE particles.To fulfill this task neutrino detectors must be design to optimise reconstruction of particle direction and energy, thus they are commonly referred as neutrino telescopes (for a clear review see [31]). 

Plugging the WB limit flux (see formula 4) into equation 8 and integrating over solid angle, one gets a rate of about 102 upgoing events per year for a 1 km2 effective area detector with E 1 TeV threshold. This number set the scale of dimension for astrophysical neutrino detectors. 

M.S. Musumeci for the NEMO Collaboration Mechanical Structures for a Deep Seawater Neutrino Detector. In VLVi/T Workshop Proc., pages 153-156, Amsterdam, 2003. Proceedings available at http / /www. vlvnt. nl /proceedings... 

Keywords Neutrino Detector, Neutrino Telescopes, Neutrino Astronomy, Antarctic Ice, Ul-... 

Because neutrinos emitted by PP reactions provide insight into processes occurring in the Solar core, experimenters have carried out numerous campaigns to detect these elusive particles. Those experiments have shown that neutrinos are indeed produced by PP reactions in the Sun, as expected, but that some of these electron-type neutrinos convert into mu-type and tau-type neutrinos on their way to Earth (4). Such neutrino conversion lies outside the Standard Model of Particle Physics thus. Earth-based neutrino detectors have not only provided stunning confirmation of the astrophysics of stars but also invaluable insights into the nature of fundamental particles (e.g., 5). 

Table 2 shows this volume for distances ranging from 1 km to an Earth diameter (12800 km). For comparison, the largest neutrino detector ever built, SuperKamiokande, contains 50,000 tons of purified water (equivalent to a cube 37 m on a side) and corresponding to a range of about 25 km. 

P. Alivisatos, et al., KamLAND, a Liquid Scintillator Anti-Neutrino Detector at the Kamioka Site, Preprint Stanford-HEP-98-03 Tohoku-RCNS-98-15 (Geneva Cem Library SCAN-9809050), at http //alice.cem.ch/search/complex uid=3470113 2649 freetextl=Alivisatos+P fieldl=wau, p. 60. 

Rubbia, C., The Liquid-Argon Time Projection Chamber A New Concept for Neutrino Detectors, CERN, EP int. Rep. 77-8, 1977. 

FIGURE 1 The chlorine ( CI) solar neutrino detector in the Homestake Gold Mine. Lead, South Dakota. 

Together, these detailed observations have established experimental neutrino astronomy, or, perhaps more appropriately, neutrino astrophysies, as a source of fundamental information relating to the internal structure and behavior of stars. As more powerfiil neutrino detectors become available and permit observation of other neutrino radiation from the sky, we expect that neutrino astronomy wiU be an increasingly valuable adjunct of the older astronomy employing electromagnetic radiation as its means of observation. 

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