ON SOLAR MODEL SOLUTIONS TO THE SOLAR-NEUTRINO PROBLEM

Without assuming any solar neutrino spectra but merely assuming pure n u(e) emissions from the Sun, neutrinos seen by the Kamiokande experime nt should produce at least 2.6 +/- 0.45 SNU in the lower threshold Hom estake experiment. This rate is compared with the total event rate of 2.55 +/- 0.25 SNU observed by the Homestake experiment which solar mod els tell us should measure not only B-8 neutrinos seen by the Kamiokan de but also uncertainty-free pep neutrinos (which contribute 0.2 SNU) as well as Be-7 neutrinos whose energies are below the Kamiokande thre shold. This comparison may imply that Be-7 neutrinos are more severely suppressed than the B-8 neutrinos with respect to the predictions of standard solar models, which cannot be explained by any known astrophy sics solution. (In particular, this argument is independent of uncerta inties in solar nuclear reaction rates.) It is also noted that the low er limit that the Kamiokande observations set on the B-8 neutrino flux restricts variations of standard solar models to require minimal rate s of 3.6 SNU for the Homestake experiment and 114 SNU for GALLEX and S AGE to achieve consistency (and still fit helioseismic data). Therefor e, variations of standard solar models as solutions to the solar neutr ino problem are inconsistent with the Homestake experiment and only ma rginally allowed by the gallium experiments. If the gallium experiment s eventually confirm a flux significantly below 114 SNU, it would seem to imply new neutrino physics.