Deduction of the solar internal structure from the sound speed profile in the sun and estimates of the solar neutrino fluxes based on the heliseismic data

根据Libbrecht等人（1990;AAA 52.080.103）和Jimenez等人（1988;AAA 45.080.041）的日震数据，通过求解控制恒星结构的基本方程，我们推断出了太阳内部的密度、压力、温度和氢分布。这种方法与标准的太阳模型完全不同，它是基于更多实验确定的数据。我们要求表面的质量和平均分子量分别与太阳质量和某一固定值相匹配作为外边界条件来求解方程。结合这些条件和适当的内边界条件，将这些方程简化为边值问题。我们检查表面的光度是否与观测值相符。通过蒙特卡罗模拟估计了声速分布上的高斯噪声的误差水平。所构建的地震模型在3sigma水平上略微满足亮度条件L (R_*)=L_*。利用这个满足L (R_*)=L_*的地震模型，我们估计了中微子的通量，发现^8B的中微子通量约为标准太阳模型的60%。这个模型似乎与神冈中微子探测实验相一致。模型的^7Be中微子通量比标准太阳模型小约20%，模型的pp-中微子通量与标准太阳模型几乎相同。我们估计氯实验（Homestake）的总中微子捕获率与镓实验（GALLEX和SAGE）相同，但由于CNO循环的贡献，我们基于标准太阳模型缩放捕获率。由此估计的捕获率分别为5.62 SNU和117 SNU，它们比观测值高3 σ误差水平。

We deduce the density, pressure, temperature, and hydrogen profiles in the solar interior by solving the basic equations governing stellar structure with the imposition that the sound speed profile is that determined by helioseismic data of Libbrecht et al. (1990 ; AAA 52.080.103) and Jimenez et al. (1988 ; AAA 45.080.041). This approach is completely different from that of the standard solar model, and is based on more experimentally well-determined data. We solve the equations by requiring that the mass and the mean molecular weight at the surface 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 are reduced to a boundary value problem. We examine whether the luminosity at the surface matches the observed value. The error levels are estimated by a Monte Carlo simulation with Gaussian noise on the sound speed profile. The seismic model thus constructed marginally satisfies the luminosity condition, L (R_*)=L_*, at the 3sigma level. Using this seismic model satisfying L (R_*)=L_*, we estimate the neutrino fluxes, and find that the ^8B neutrino flux is about 60% of that of the standard solar model. This model seems consistent with the Kamiokande neutrino detection experiment. The ^7Be neutrino flux of the model is about 20% smaller than the standard solar model, and the pp-neutrino flux of the model is almost the same as that of the standard solar model. We estimate the total neutrino capture rate of the chlorine experiment (Homestake) that of the gallium experiments (GALLEX and SAGE) but for a contribution from the CNO cycle by scaling the capture rates based on the standard solar model. The capture rates thus estimated are 5.62 SNU and 117 SNU,respectively, and they are higher than the observations by the 3sigma error level.