利用积分光谱确定双星比例的方法
Determination method of binary fractions by the integrated spectrum
AI总结：
本文提出一种利用积分光谱吸收特征指数沿径向累加双星比例变化来确定致密或遥远恒星系统双星比例的方法，并在银河系球状星团中验证了其可行性，同时分析了双星比例与多种星族参数的相关性。
摘要：
我们需要分辨恒星系统中的单颗恒星才能确定其双星比例。因此，对于致密或遥远的恒星系统，无法直接获得其双星比例。我们提出了一种确定致密或遥远恒星系统双星比例的方法。该方法首先确定任意两个相邻区域之间的双星比例变化，然后沿径向方向将这些双星比例变化累加，从而得到整个恒星系统的双星比例。双星比例变化通过使用十个对双星比例敏感的光谱吸收特征指数（SAFIs）以及基于这些SAFIs建立的双星比例变化定标关系来导出。利用该方法，我们首次给出了二十一个银河系球状星团（GCs）的双星比例变化。通过比较，我们发现这些结果与先前研究基于主序基准线方法得到的双星比例吻合良好。这验证了上述方法是可行的。接下来，我们给出了十三个银河系球状星团的双星比例变化。我们给出了双星比例与各种参数之间的关系，发现双星比例与NHB和NRR呈负相关，某些研究中的双星比例与NBS没有强相关性，并且在极端蓝水平分支星族比例较大的情况下，具有大双星比例的球状星团数量更多。最后，如果我们希望获得更准确的双星比例，我们建议对恒星系统在适当的区域间隔内进行光谱和测光观测。
英文摘要：
We need to resolve the individual stars for binary fraction determinations of stellar systems. Therefore, it is not possible to obtain the binary fractions for dense or distant stellar systems. % We proposed a method to determine the binary fraction of a dense or distant stellar system. The method is to first determine the binary fraction variation for any two adjacent regions and then add up those binary fraction variations along the radial direction to obtain the binary fraction for a stellar system. Binary fraction variation is derived by using ten binary fraction-sensitive spectral absorption feature indices (SAFIs) and the binary fraction variation calibrations in terms of these SAFIs. Using this method, we first presented the binary fraction variations for twenty-one Galactic globular clusters (GCs). By comparisons, we find that they agree well with the binary fractions based on the main-sequence fiducial line method by previous studies. This verifies that the above mentioned method is feasible. Next, we presented the binary fraction variations of thirteen Galactic GCs. We gave the relationships between binary fraction and various parameters, and found that binary fraction is negatively correlated with NHB and NRR, binary fraction of some studies is not strongly correlated with NBS, and the number of GCs with large binary fraction is greater at extreme blue horizontal branch population ratio. At last, if we want to obtain more accurate binary fraction, we suggest that the spectroscopic and photometric observations are conducted at an appropriate area interval for a stellar system.
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