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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

从太阳声速剖面推导出太阳内部结构，并根据日震数据估计太阳中微子通量

基本信息

批准号：
06452018
负责人：
SHIBAHASHI Hiromoto
金额：
$ 4.74万
依托单位：
The University of Tokyo
依托单位国家：
日本
项目类别：
Grant-in-Aid for General Scientific Research (B)
财政年份：
1994
资助国家：
日本
起止时间：
1994 至 1995
项目状态：
已结题

来源：
https://kaken.nii.ac.jp/en/grant/KAKENHI-PROJECT-06452018/
关键词：
Sun ; internal Structure Sun ; Oscillation Helioseismology Solar Neutrinos

项目摘要

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.

我们通过求解控制恒星结构的基本方程，推导出太阳内部的密度、压力、温度和氢的分布，并假定声速分布是由Libbrecht等人（1990 ; AAA 52.080.103）和Jimenez等人（1988 ; AAA 45.080.041）的日震数据确定的。这种方法与标准太阳模型完全不同，并且基于更多的实验确定的数据。我们求解方程，要求在表面的质量和平均分子量匹配太阳质量和一定的固定值，分别作为外边界条件。加上这些条件和适当的内边界条件，这些方程被减少到一个边值问题。我们检查表面的光度是否与观测值相匹配。的误差水平估计的Monte Carlo模拟与高斯噪声的声速剖面。由此构造的地震模型在3sigma水平上勉强满足亮度条件L（R *）=L *。利用这个满足L（R *）=L * 的地震模型，我们估算了中微子流量，发现^8B中微子流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一致。该模型的^7Be中微子通量比标准太阳模型小约20%，而pp中微子通量与标准太阳模型几乎相同。我们估计总的中微子捕获率的氯实验（Homestake）的镓实验（GALLEX和SAGE），但从CNO循环的贡献缩放捕获率的基础上的标准太阳能模型。由此估计的捕获率分别为5.62 SNU和117 SNU，并且它们比观测值高3sigma误差水平。