Nuclear reaction rates are crucial ingredients of solar and stellar models, they directly impact the duration of the life of stars and the energy they produce. In the solar case, the tight observational constraints put on models (Mass, Radius, Luminosity and chemical composition) coupled to our capabilities to probe the solar interior thanks to helioseismology and solar neutrinos provide an exquisite testbed for such physical ingredients. With the recent publication of the Solar Fusion III reaction rates, a new generation of solar models may be computed and put to the test. We aim to investigate the impact of the new Solar Fusion III reaction rates on solar models, both standard and non-standard, as well as the impact of the current uncertainties on some key solar reactions on the predicted neutrino fluxes for boron and the so-called CNO cycle. We compute various theoretical standard solar models as well as non-standard models reproducing the depletion of lithium and beryllium for various abundances, nuclear reaction rates and opacities. We focus on the impact of the solar fusion III reaction rates on both helioseismic inversion results and neutrino fluxes. We find that using the Solar Fusion III reaction rates significantly impact the agreement of solar models both with helioseismic constraints and neutrino flux measurements. While for helioseismic constraints it seems that there is a slight improvement, for neutrino fluxes, the use of the SFIII reaction rates induces a lowering of the beryllium, boron and CNO neutrino fluxes. When investigating the impact of changes on the rates of key reactions within their quoted uncertainties, we find that these changes are far from sufficient to reconcile models and observations, potentially hinting at other processes (e.g. planetary formation as found in other studies).
Rotating Solar Models in Agreement with Helioseismic Results and Updated Neutrino Fluxes
根据旧的太阳丰度构造的标准太阳模型（SSM）与地震推断的结果合理一致，但新的低金属丰度的SSM与地震推断的结果不一致。中微子通量对太阳模型的约束与日震结果的约束是平行存在的。太阳中微子通量由Borexino合作组织更新。我们构建了新的低金属丰度的增强扩散和对流过冲的影响，包括旋转太阳模型。一个旋转模型使用蛋白石不透明度和卡福丰度尺度有更好的声速和密度剖面比SSM与旧的太阳丰度和再现观测到的$p$模式频率比$r_{02}$和$r_{13}$。在$1σ$水平上，模型对流带的深度和氦丰度与地震推断的结果一致。更新后的中微子通量也被模型在$1σ$水平上再现。旋转和增强扩散的影响不仅改善了模型的声速和密度分布，但使中微子通量预测模型与检测到的一致。此外，计算表明，OP可能会低估太阳区域的不透明度与$T\gtrsim5\times10^{6}$ K约$1.5\%$，而OPAL可能会低估太阳区域的不透明度与$2\times10^{6}$ K $\lesssim T \lesssim 5\times10^{6}$ K约$1-2\%$。
Investigating Energetic X-Shaped Flares on the Outskirts of A Solar Active Region
典型的太阳耀斑在色球层上显示出两条准平行的明亮带状物。在它们之间的是极性反转线（PIL），其分离有源区（AR）中相反极性的集中磁通量。有趣的是，在NOAA AR 11967外围的类似位置也发生了一系列X形条带的耀斑，那里的磁通量分散，但其中三个耀斑的能量惊人。X形状，其中心与硬X射线发射重合，在UV/EUV中是相似的，这在标准耀斑模型中是不能容纳的。绘制出势场中的磁连通性，我们发现X形态由两个准分界线层的交叉决定，即，双曲线通量管（HFT），其中嵌入连接双零的分离器。这种拓扑结构不是纯粹的局部，而是受整个AR的通量和流量的调节。非线性无力场模型建议在HFT处形成电流层，其中电流耗散可以通过场对准热传导映射到X形带。这些结果突出了高频电磁场在三维磁重联中的关键作用，并对天体物理和实验室等离子体具有重要意义。
