论文标题
旋转太阳能模型与Helioseiscic结果一致并更新中微子通量
Rotating Solar Models in Agreement with Helioseismic Results and Updated Neutrino Fluxes
论文作者
论文摘要
根据旧太阳丰度构建的标准太阳能模型（SSM）与地震上推断出的结果是合理的，但是具有新的低金属丰度的SSM与地震上推断的结果不同意。中微子通量在太阳模型上的限制与Helioseiscic结果并行存在。太阳中微子通量由Borexino Collaboration更新。我们构建了具有新的低金属丰度的旋转太阳能模型，其中包括增强的扩散和对流的影响。使用蛋白石不透性和Caffau丰度量表的旋转模型比具有旧太阳丰度的SSM具有更好的声速和密度曲线，并重现了观察到的$ p $ mmode频率比$ r_ {02} $和$ r_ {13} $。模型对流区的深度和氦气丰度与$1σ$的地震级别推断的深度相吻合。更新的中微子通量也由$1σ$的级别复制。旋转和增强扩散的影响不仅可以改善模型的声速和密度曲线，而且使模型预测的中微子通量与检测到的中微子通量一致。此外，计算表明，OP可能会低估$ t \ gtrsim5 \ times10^{6} $ k的阳光区域的不透明，约1.5美元左右，而蛋白石可能低估了$ 2 \ times10^$ k $ k $ k $ k $ k $ k $ k $ k $ k $ k $ k $ k $ k $ k $ k $ k $ k $ k $ \ bsim times time time time time time time time time times time time time timessim timessim timessim timessim timessim。 $ 1-2 \％$。
Standard solar models (SSMs) constructed in accordance with old solar abundances are in reasonable agreement with seismically inferred results, but SSMs with new low-metal abundances disagree with the seismically inferred results. The constraints of neutrino fluxes on solar models exist in parallel with those of helioseismic results. The solar neutrino fluxes were updated by Borexino Collaboration. We constructed rotating solar models with new low-metal abundances where the effects of enhanced diffusion and convection overshoot were included. A rotating model using OPAL opacities and the Caffau abundance scale has better sound-speed and density profiles than the SSM with the old solar abundances and reproduces the observed $p$-mode frequency ratios $r_{02}$ and $r_{13}$. The depth and helium abundance of the convection zone of the model agree with the seismically inferred ones at the level of $1σ$. The updated neutrino fluxes are also reproduced by the model at the level of $1σ$. The effects of rotation and enhanced diffusion not only improve the model's sound-speed and density profiles but bring the neutrino fluxes predicted by the model into agreement with the detected ones. Moreover, the calculations show that OP may underestimate opacities for the regions of the Sun with $T\gtrsim5\times10^{6}$ K by around $1.5\%$, while OPAL may underestimate opacities for the regions of the Sun with $2\times10^{6}$ K $\lesssim T \lesssim 5\times10^{6}$ K by about $1-2\%$.
