Astronomy and Astrophysics for the 1980's, Volume 2 Reports of the Panels (1983) / Chapter Skim
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IX. Neutrino Astronomy
IX. Neutrino Astronomy
Pages 84-89
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From page 84... ...
To obtain a significant rate of detectable interactions a detector must have a very great number of target nuclei in its sensitive volume, which means that it So far, the only positive detection cosmic sources has been of low-energy neutrinos produced in the nearest star, the Sun. Efforts are under way, or under consideration, to detect cosmic neutrinos in the intermediate- and high-energy regimes.
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From page 85... ...
. The current standard theoretical model for the Sun predicts a counting rate of 7.5 SNUS, with a considerable uncertainty due to uncertainties in the nuclear cross sections, the optical opacities, and the conditions in the Sun's core.
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From page 86... ...
Measurement of the energy spectrum of the solar neutrinos will then become the next major objective. m e most promising approach to the measurement of the pp neutrinos is the so-called ~gallium" experiment, which, like the 37C1 experiment, is a radiochemical experiment with 71Ga being the target nucleus and 71Ge being the separable radioactive product nucleus.
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From page 87... ...
Introduction The most easily detectable contributions to the neutrino flux in the intermediate-energy range from 10 to 50 MeV are expected to come from gravitational collapses of stars in our Galaxy, which occur with an estimated frequency of one per 10 to 30 years. Although many details of collapse processes are uncertain, there is general agreement on several theoretical conclusions.
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From page 88... ...
3. Scientific Goals and Future Programs Existing facilities capable of detecting neutrinos from stellar collapse events in our Galaxy should be adequately maintained and operated for many years.
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From page 89... ...
Upper limits on the diffuse cosmic neutrino flux have been obtained with detectors located deep underground in gold mines in India, South Africa, and the United States. These limits place significant constraints on the amount of deuterium that was produced after the initial element synthesis in the big bang.
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