使用经验混合长度校准的$α$半人马座A和B的经典和星震约束的1D恒星演化模型
Classically and Asteroseismically constrained 1D Stellar Evolution Models of $α$ Centauri A and B using Empirical Mixing Length Calibrations
摘要：
明亮的，附近的双星$α$ Centauri为测试恒星演化模型提供了一个很好的实验室，因为它是我们拥有高精度经典（质量，半径，光度）和星震（$p$模式）观测的少数恒星系统之一。恒星模型的创建和适合的经典和地震观测的两颗星，允许对流混合长度参数$α_{\text{MLT}}$的自由变化。这个系统的建模使用五套不同的假设的物理支配恒星模型。在$3\,σ$中，有31对符合系统的经典、二元和地震观测约束的轨迹（在生成的${\sim} 150,000$之外）。模型与每个测试的输入物理选择被认为是可行的，但最佳的混合长度为Cen A和Cen B保持不变，无论物理处方。最佳混合长度为$α_{\text{MLT,A}} /α_{\odot}= 0.932$和$α_{\text{MLT,B}}/α_{\odot} = 1.095$。Cen A和Cen B分别需要亚太阳和超太阳混合长度来拟合观测结果，这一趋势与最近的发现一致，例如Kervella et al.（2017），Joyce and Chaboyer（2018）和Viani et al.（2018）。最佳模型发现的年龄为$5.3 \pm 0.3$陀螺仪的$α$半人马座。
英文摘要：
The bright, nearby binary $α$ Centauri provides an excellent laboratory for testing stellar evolution models, as it is one of the few stellar systems for which we have high-precision classical (mass, radius, luminosity) and asteroseismic ($p$-mode) observations. Stellar models are created and fit to the classical and seismic observations of both stars by allowing for the free variation of convective mixing length parameter $α_{\text{MLT}}$. This system is modeled using five different sets of assumptions about the physics governing the stellar models. There are 31 pairs of tracks (out of ${\sim} 150,000$ generated) which fit the classical, binary, and seismic observational constraints of the system within $3\,σ$. Models with each tested choice of input physics are found to be viable, but the optimal mixing lengths for Cen A and Cen B remain the same regardless of the physical prescription. The optimal mixing lengths are $α_{\text{MLT,A}} /α_{\odot}= 0.932$ and $α_{\text{MLT,B}}/α_{\odot} = 1.095$. That Cen A and Cen B require sub- and super-solar mixing lengths, respectively, to fit the observations is a trend consistent with recent findings, such as in Kervella et al. (2017), Joyce and Chaboyer (2018), and Viani et al. (2018). The optimal models find an age for $α$ Centauri of $5.3 \pm 0.3$ Gyr.
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