论文标题
太阳中微子通量的行星形成过程的签名的证据
Evidence of a signature of planet formation processes from solar neutrino fluxes
论文作者
论文摘要
到目前为止，太阳进化模型无法始终如一地重现光谱，热震和中微子约束，从而导致所谓的太阳建模问题。同时，行星形成模型可以预测，原始磁盘的不断发展的组成，因此由原始磁盘积聚的气体成分必须是可变的。我们表明，包括逼真的行星形成场景的太阳进化模型导致高达5％的核心金属性增加，这意味着准确的中微子通量测量值对太阳系形成的初始阶段敏感。具有同质积聚的模型中微子约束的模型不超过2.7 $σ$。相比之下，由于行星形成过程而产生的可变成分的积聚，导致最后$ \ sim的金属贫困积聚，$ \ sim $ 4％的年轻太阳总质量的4％，在所有中等基础约束的1.3 $σ$之内产生太阳能模型。因此，我们证明，除了增加对流包络底部的不相处外，太阳系的形成历史还构成了解决当前太阳能模型危机的关键要素。
Solar evolutionary models are thus far unable to reproduce spectroscopic, helioseismic, and neutrino constraints consistently, resulting in the so-called solar modeling problem. In parallel, planet formation models predict that the evolving composition of the protosolar disk and, thus, of the gas accreted by the proto-Sun must have been variable. We show that solar evolutionary models that include a realistic planet formation scenario lead to an increased core metallicity of up to 5%, implying that accurate neutrino flux measurements are sensitive to the initial stages of the formation of the Solar System. Models with homogeneous accretion match neutrino constraints to no better than 2.7$σ$. In contrast, accretion with a variable composition due to planet formation processes, leading to metal-poor accretion of the last $\sim$4% of the young Sun's total mass, yields solar models within 1.3$σ$ of all neutrino constraints. We thus demonstrate that in addition to increased opacities at the base of the convective envelope, the formation history of the Solar System constitutes a key element in resolving the current crisis of solar models.
