Solar models based on helioseismology and the solar neutrino problem

We have determined the sound-speed profile in the Sun by carrying out an as ymptotic inversion of the helioseismic data from the Low-Degree (I) Oscilla tion Experiment (LOWL), the Global Oscillation Network Group (GONG), VIRGO on SOHO, the High-l Helioseismometer (HLH), and observations made at the So uth Pole. We then deduce the density, pressure, temperature, and elemental composition profiles in the solar radiative interior by solving the basic e quations governing the stellar structure, with the imposition of the determ ined sound-speed profile and with a constraint on the depth of the convecti on zone obtained from helioseismic analysis and the ratio of the metal abun dance to the hydrogen abundance at the photosphere. With the exception of t he treatment of elements relevant to nuclear reactions, we assume that Z is homogeneous. The chemical composition profiles of hydrogen and helium are then obtained as a part of the solutions. Using the resulting seismic model , we estimate the neutrino fluxes and the neutrino capture rates for the ch lorine, gallium, and water Cerenkov experiments. Even if we take into accou nt uncertainties in various input physics, the estimated capture rates are still significantly larger than the observation.