论文标题
太阳能质子 - 蛋白质融合反应速率及其不确定性的理论评估
Theoretical evaluation of solar proton-proton fusion reaction rate and its uncertainties
论文作者
论文摘要
弱质子 - 蛋白质融合到杜特隆（$^2 $ h）是太阳能量产生中的驱动反应以及类似的主序列。其在太阳内部的反应速率仅在理论上确定。在这里，我们使用有效的量子染色体式动力学的有效现场理论，在近代到领先的顺序上使用量子染色体的有效现场理论，对在太阳条件下的速率进行了新的确定，并分析了不确定性的理论和实验来源。我们发现$ s^{11} $的增强额为$ 1-4 \％$ $，而不是先前推荐的值。这种变化减少了源自$^8 $ b的中心渠的计算通量，$^7 $是阳光下的核反应，因此有利于金属光谱元素的更高丰度，在不同的组成确定之间的张力（称为````solar构图'''''之间的张力。
The weak proton-proton fusion into a deuteron ($^2$H) is the driving reaction in the energy production in the Sun, as well as similar main sequence stars. Its reaction rate in the solar interior is determined only theoretically. Here, we provide a new determination of the rate of this reaction in solar conditions $S^{11}(0)$, and analyze theoretical and experimental sources for uncertainties, using effective field theory of quantum chromo-dynamics without explicit pions at next-to-leading order. We find an enhancement of $S^{11}$ by $1-4\%$ over the previously recommended value. This change reduces the calculated fluxes of neutrinos originating in $^8$B and $^7$Be nuclear reactions in the Sun, thus favoring higher abundances for metallic photospheric elements, in the tension between different composition determination, known as the ``Solar Composition Problem''.
