A SEISMIC SOLAR MODEL DEDUCED FROM THE SOUND-SPEED DISTRIBUTION AND AN ESTIMATE OF THE NEUTRINO FLUXES

We have deduced the density, pressure, temperature, and hydrogen profi les in the solar interior by solving the basic equations governing the stellar structure with the imposition that the sound-speed profile is that determined by the helioseismic data of Libbrecht et al. (1990; A AA 52.080.103) and Jimenez et al. (1988; AAA 45.080.041). This approac h is completely different from that of the standard solar model, and i s based on more experimentally well-determined data. We solved the equ ations by requiring that the mass and mean molecular weight at the sur face match the solar mass and a certain fixed value, respectively, as the outer boundary conditions. Together with these conditions and the appropriate inner boundary conditions, these equations were reduced to a boundary-value problem. We examined whether the luminosity at the s urface matches the observed value. The error levels were estimated by a Monte-Carlo simulation with Gaussian noise on the sound-speed profil e. The thus-constructed seismic model marginally satisfies the luminos ity condition, L(R.) = L., at the 3 sigma level. Using this seismic mo del, we estimated the neutrino fluxes, and found that the B-8 neutrino flux is about 60% of that of the standard solar model. This model doe s not seem to contradict the Kamiokande neutrino detection experiment. The Be-7 neutrino flux of the model is about 20% smaller than the sta ndard solar model, and the pp-neutrino flux of the model is almost the same as that of the standard solar model. We estimated the total neut rino capture rate of the chlorine experiment (Homestake) and that of t he gallium experiments (GALLEX and SAGE), except for a contribution fr om the CNO cycle, by scaling the capture rates based on the standard s olar model. The thus-estimated capture rates are 5.62 SNU and 117 SNU, respectively, and are higher than those observed at the 3 sigma error level.