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Can the measurement of the cross-section of proton-capture on beryllium-7 be improved [electronic resource].

Published:
Washington, D.C. : United States. Dept. of Energy, 1993.
Oak Ridge, Tenn. : Distributed by the Office of Scientific and Technical Information, U.S. Dept. of Energy.
Physical Description:
Pages: (17 pages) : digital, PDF file
Additional Creators:
Lawrence Berkeley National Laboratory, United States. Department of Energy, and United States. Department of Energy. Office of Scientific and Technical Information
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Summary:
The solar neutrino problem'' arises from the discrepancy between the observations of solar neutrinos fluxes in experiments at Homestake and Kamiokande and the solar model predictions of those fluxes. Both experiments, which are sensitive mainly to high-energy neutrinos, observe fewer neutrinos than predicted by solar models. Most of the expected high-energy solar neutrinos come from the beta-decay of [sup 8]B, which is produced in the reaction [sup 7]Be(p,[gamma])[sup 8]B. A study of all of the measurements to date of the zero-energy S-factor for the reaction [sup 7]Be(p,[gamma])[sup 8]B concludes that S[sub 17](0) = 0.0224 +[plus minus] 0.0021 keV-barn. Although a 10% error in S[sub 17](0) alone wig not solve the solar neutrino problem, it would still be useful to nail down all of the inputs of the solar models as well as possible. This serves to guard against the possibility that a conspiracy among the errors might be the source of the discrepancy and provides tighter constraints on the new physics'' interpretations of the experimentally measured solar neutrino spectrum. In this paper, we examine several ways of improving this measurement. None appear to offer a significant improvement over past experiments.
Report Numbers:
E 1.99:lbl-33573
lbl-33573
Subject(s):
Other Subject(s):
Note:
Published through SciTech Connect.
01/01/1993.
"lbl-33573"
"DE93015261"
Bowers, C.
Funding Information:
AC03-76SF00098
View MARC record | catkey: 14670456