用CHARA阵列干涉测量的G亚矮星$μ$ Cassiopeiae A和K矮星PDMATHAAB Draconis和HR 511的角直径
Angular Diameters of the G Subdwarf $μ$ Cassiopeiae A and the K Dwarfs $σ$ Draconis and HR 511 from Interferometric Measurements with the CHARA Array
摘要：
利用CHARA阵列的最长基线，我们测量了G5 V亚矮星$μ$ Cas A的角直径，这是第一次对晕族星进行这样的测定。我们将这一结果与金属丰度较高的K0 V型恒星$σ$ Dra和HR 511的新直径进行比较，发现贫金属恒星$μ$ Cas A的有效温度（$T_{\rm eff}=5297\pm32$ K）、半径（$R=0.791\pm0.008 R_{\rm \odot}$）和绝对光度（$L=0.442\pm0.014 L_{\rm \odot}$）与其他两颗光谱类型较晚的恒星相当。我们发现，恒星模型显示的差异，预测的温度和半径为$μ$ Cas A，我们讨论这些结果，以及它们如何提供一个关键的理解低金属量的恒星的基本关系。
英文摘要：
Using the longest baselines of the CHARA Array, we have measured the angular diameter of the G5 V subdwarf $μ$ Cas A, the first such determination for a halo population star. We compare this result to new diameters for the higher metallicity K0 V stars, $σ$ Dra and HR 511, and find that the metal-poor star, $μ$ Cas A, has an effective temperature ($T_{\rm eff}=5297\pm32$ K), radius ($R=0.791\pm0.008 R_{\rm \odot}$), and absolute luminosity ($L=0.442\pm0.014 L_{\rm \odot}$) comparable to the other two stars with later spectral types. We show that stellar models show a discrepancy in the predicted temperature and radius for $μ$ Cas A, and we discuss these results and how they provide a key to understanding the fundamental relationships for stars with low metallicity.
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