Solar Neutrinos: What We Have Learned

Details Solar Neutrinos: What We Have Learned Solar Neutrinos: What We Have Learned

1993-12-02

arxiv.org/abs/astro-ph/9312002v1

in Physical Processes in Astrophysics, proceedings of the International Meeting in Honour of Evry Schatzman, September 1993, P

Astronomy and Astrophysics

Astrophysics

LaTeX file, 19 pages. For hardcopy with figures contact BEST@SNS.IAS.EDU. Institute for Advanced Study number AST 93/69

Scientific paper

The four operating solar neutrino experiments confirm the hypothesis that the energy source for solar luminosity is hydrogen fusion. However, the measured rate for each of the four solar neutrino experiments differs significantly (by factors of 2.0 to 3.5) from the corresponding theoretical prediction that is based upon the standard solar model and the simplest version of the standard electroweak theory. If standard electroweak theory is correct, the energy spectrum for \b8 neutrinos created in the solar interior must be the same (to one part in $10^5$) as the known laboratory \b8 neutrino energy spectrum. Direct comparison of the chlorine and the Kamiokande experiments, both sensitive to \b8 neutrinos, suggests that the discrepancy between theory and observations depends upon neutrino energy, in conflict with standard expectations. Monte Carlo studies with 1000 implementations of the standard solar model confirm that the chlorine and the Kamiokande experiments cannot be reconciled unless new weak interaction physics changes the shape of the \b8 neutrino energy spectrum. The results of the two gallium solar neutrino experiments strengthen the conclusion that new physics is required and help determine a relatively small allowed region for the MSW neutrino parameters.

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