解纠缠双星谱的约束拟合：应用于疏散星团h英仙座的V615 Per
Constrained fitting of disentangled binary spectra: application to V615 Per in the open cluster h Persei
摘要：
利用光谱解缠技术，可以从在一系列轨道相位观测到的复合光谱中确定多星系统各组成部分的单独光谱。这种方法有几个优点：它不受线混合的影响，不使用模板光谱，并返回具有非常高的信噪比的单个组分光谱。双星系统的解纠缠光谱非常适合光谱分析，但有一个问题：绝对谱线深度是未知的，因为这一信息不包含在原始光谱中（除非有一个在日食），而不对组成恒星的光谱特征进行假设。本文提出了一种用合成光谱对观测光谱和解纠缠光谱进行约束拟合，从而获得组成星大气参数的方法。解纠缠光谱拟合使用合成光谱和遗传算法，以确定有效的温度，表面重力和相对光的贡献的两颗恒星在一个二元系统。该方法被证明在合成光谱，然后应用到食双星V615 Per，年轻的疏散星团NGC 869（h英仙座）的成员。该方法对于信噪比为100或更高的解纠缠光谱工作良好。对于V615 Per，我们发现一个正常的He丰度，但Mg丰度，这表明散装金属丰度，比附近的OB星典型的低两个因素。
英文摘要：
Using the technique of spectral disentangling, it is possible to determine the individual spectra of the components of a multiple star system from composite spectra observed at a range of orbital phases. This method has several advantages: it is unaffected by line blending, does not use template spectra, and returns individual component spectra with very high signal-to-noise ratios. The disentangled spectra of a binary star system are very well suited to spectroscopic analysis but for one problem: the absolute spectral line depths are unknown because this information is not contained in the original spectra (unless there is one taken in eclipse) without making assumptions about the spectral characteristics of the component stars. Here we present a method for obtaining the atmospheric parameters of the component stars by the constrained fitting of synthetic spectra to observed and disentangled spectra. Disentangled spectra are fitted using synthetic spectra and a genetic algorithm in order to determine the effective temperatures, surface gravities and relative light contributions of the two stars in a binary system. The method is demonstrated on synthetic spectra and then applied to the eclipsing binary V615 Per, a member of the young open cluster NGC 869 (h Persei). The method works well for disentangled spectra with signal-to-noise ratios of 100 or more. For V615 Per we find a normal He abundance but an Mg abundance, which indicates bulk metallicity, a factor of two lower than typical for nearby OB stars.
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