Represents the Energy Taken Away By Neutrinos, With an Average Value Being

The Sun is a main-sequence star at a stage of stable hydrogen burning. It produces an intense ux of electron neutrinos as a consequence of nuclear fusion reactions which generate solar energy, and whose combined eeect is 4p + 2e ? ! 4 He + 2 e + 26:73 MeV ? E ; (1) where E represents the energy taken away by neutrinos, with an average value being hE i 0:6 MeV. Each neutrino-producing reaction, the resulting ux, and contributions to the event rates in chlorine and gallium solar-neutrino experiments predicted by the recent Bahcall and Pinsonneault standard solar model (SSM) calculation 1] are listed in Table 1. This SSM is regarded as the best with helium and heavy-element diiusion. Figure 1 shows the energy spectra of solar neutrinos from these reactions quoted from the SSM calculation by Bahcall and Ulrich 2]. Recently, the SSM has been shown to predict accurately the helioseismological sound velocities with a precision of 0.1% rms throughout essentially the entire Sun, greatly strengthening the conndence in the solar model 3]. Observation of solar neutrinos directly addresses the SSM and, more generally, the theory of stellar structure and evolution which is the basis of the SSM. The Sun as a well-deened neutrino source also provides extremely important opportunities to investigate nontrivial neutrino properties such as nonzero mass and mixing, because of the wide range of matter density and the very long distance from the Sun to the Earth. In fact, the currently available solar-neutrino data seem to require such neutrino properties, if one tries to understand them consistently. So far, four solar-neutrino experiments published the results. In addition, a new solar-neutrino experiment (Super-Kamiokande) started observation in 1996.