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arXiv 0909.2668astro-ph.SRhep-ph
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新的太阳成分：太阳模型的问题再访

New Solar Composition: The Problem With Solar Models Revisited

Aldo Serenelli, Sarbani Basu, Jason W. Ferguson, Martin Asplund

备注：
Accepted for publication in ApJ Letters. Changes according to referee's comments. 11 pages, including 3 tables and 2 figures
发表信息：
Astrophys.J.705:L123-L127,2009
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摘要：

我们用不同的太阳丰度组构建了更新的太阳模型，包括Asplund等人（2009）的最新测定。后一项工作预测太阳金属丰度（$\sim 10%$）比同一作者以前的测量值更大，但（$\sim 25%$）比Grevesse & Sauval（1998）十年前的建议值要低得多。我们比较我们的模型的结果与通过日震学测量推断的太阳结构的测定。使用最新太阳丰度测定的模型预测太阳对流包层的底部位于$R_{\rm CZ}= 0.724{\rm R_\odot}$，表面氦的质量分数为$Y_{\rm surf}=0.231$。这些结果与日震学资料（$R_{\rm CZ}= 0.713\pm0.001{\rm R_\odot}$和$Y_{\rm surf}=0.2485\pm0.0035$）分别在5个和11个$-σ$水平上存在矛盾。使用新的太阳丰度，我们计算的幅度，辐射不透明度应修改，以恢复与日震学的协议。我们发现，在对流区的底部的最大变化的$\sim 15%$需要一个平滑的减少向核心，其中所需的变化是$\sim 5%$。对流包络底部所需的变化约为先前估计值的一半。我们还介绍了新模型预测的太阳中微子通量。新的太阳丰度带来的最重要的变化是增加了$\sim 10%$在预测的$^{13}$ N和$^{15}$ O通量，主要是由于在新确定的太阳组成的C和N丰度的增加。

英文摘要：

We construct updated solar models with different sets of solar abundances, including the most recent determinations by Asplund et al. (2009). The latter work predicts a larger ($\sim 10%$) solar metallicity compared to previous measurements by the same authors but significantly lower ($\sim 25%$) than the recommended value from a decade ago by Grevesse & Sauval (1998). We compare the results of our models with determinations of the solar structure inferred through helioseismology measurements. The model that uses the most recent solar abundance determinations predicts the base of the solar convective envelope to be located at $R_{\rm CZ}= 0.724{\rm R_\odot}$ and a surface helium mass fraction of $Y_{\rm surf}=0.231$. These results are in conflict with helioseismology data ($R_{\rm CZ}= 0.713\pm0.001{\rm R_\odot}$ and $Y_{\rm surf}=0.2485\pm0.0035$) at 5$-σ$ and 11$-σ$ levels respectively. Using the new solar abundances, we calculate the magnitude by which radiative opacities should be modified in order to restore agreement with helioseismology. We find that a maximum change of $\sim 15%$ at the base of the convective zone is required with a smooth decrease towards the core, where the change needed is $\sim 5%$. The required change at the base of the convective envelope is about half the value estimated previously. We also present the solar neutrino fluxes predicted by the new models. The most important changes brought about by the new solar abundances are the increase by $\sim 10%$ in the predicted $^{13}$N and $^{15}$O fluxes that arise mostly due to the increase in the C and N abundances in the newly determined solar composition.

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