元素扩散的模拟$ε$ Eridani和星震试验
Modeling $ε$ Eridani and asteroseismic tests of element diffusion
摘要：
考虑到氦和金属的扩散，我们探索了可能的演化状态，并进行了地震分析的MOST目标：恒星$ε$波江座。我们采用不同的输入参数，通过拟合可用的观测约束来构建模型：例如，$T_{eff}$、$L$、$R$、$[Fe/H]$。通过计算，我们得到了$ε$波江座在$194\pm 1 μ$ Hz附近的平均大间距.扩散模型的年龄已被发现是约1 Gyr，这是年轻的比以前确定的模型没有扩散。我们发现纯氦扩散对年轻低质量恒星内部结构的影响很小，而金属扩散的影响很明显。金属的扩散导致模型辐射内部的温度更高，相应地，模型内部的声速更高，从而更大的频率和间距。
英文摘要：
Taking into account the helium and metal diffusion, we explore the possible evolutionary status and perform seismic analysis of MOST target: the star $ε$ Eridani. We adopt the different input parameters to construct the models by fitting the available observational constraints: e.g., $T_{eff}$, $L$, $R$, $[Fe/H]$. From computation, we obtain the average large spacings of $ε$ Eridani about $194\pm 1 μ$Hz. The age of the diffused models has been found to be about 1 Gyr, which is younger than one determined previously by models without diffusion. We found that the effect of pure helium diffusion on the internal structure of the young low-mass star is slight, but the metal diffusion influence is obvious. The metal diffusion leads the models to have much higher temperature in the radiation interior, correspondingly the higher sound speed in the interior of the model, thereby the larger frequency and spacings.
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