探索双星配对算法的结果
Exploring the consequences of pairing algorithms for binary stars
摘要：
恒星群中的双星数量的知识提供了关于不同环境中恒星形成过程结果的重要信息（参见，例如，Blaauw 1991，以及其中的参考文献）。双星性也是恒星星族研究中的一个关键因素，是校准双星演化通道的前提。在本文中，我们提出了一个概述的几种常用的方法来配对单个恒星到双星系统，我们称之为配对函数。这些配对函数经常被观测者和计算天文学家使用，或者是为了数学上的方便，或者是因为它们粗略地描述了恒星形成过程的预期结果。我们讨论的后果，每个配对函数的解释观测和数值模拟。二元分数和质量比分布通常强烈依赖于样品中主要光谱类型范围的选择。因此，从质量有限的目标样本中的二元性调查得出的质量比分布和二元分数并不代表整个群体。无论是理论还是观测都没有表明，从质量分布中随机配对的二元组分，最简单的配对函数，是现实的。更有可能的是伴星是在恒星周围的圆盘中形成的，或者是前双星核心分裂成两个双星。我们的分析结果是很重要的（一）所观察到的质量比分布和二进制分数的恒星样本的解释，（ii）一系列可能的初始条件算法的星团模拟，以及（iii）如何区分不同的恒星形成的情况。
英文摘要：
Knowledge of the binary population in stellar groupings provides important information about the outcome of the star forming process in different environments (see, e.g., Blaauw 1991, and references therein). Binarity is also a key ingredient in stellar population studies, and is a prerequisite to calibrate the binary evolution channels. In this paper we present an overview of several commonly used methods to pair individual stars into binary systems, which we refer to as pairing functions. These pairing functions are frequently used by observers and computational astronomers, either for their mathematical convenience, or because they roughly describe the expected outcome of the star forming process. We discuss the consequences of each pairing function for the interpretation of observations and numerical simulations. The binary fraction and mass ratio distribution generally depend strongly on the selection of the range in primary spectral type in a sample. The mass ratio distribution and binary fraction derived from a binarity survey among a mass-limited sample of targets is thus not representative for the population as a whole. Neither theory nor observations indicate that random pairing of binary components from the mass distribution, the simplest pairing function, is realistic. It is more likely that companion stars are formed in a disk around a star, or that a pre-binary core fragments into two binary components. The results of our analysis are important for (i) the interpretation of the observed mass ratio distribution and binary fraction for a sample of stars, (ii) a range of possible initial condition algorithms for star cluster simulations, and (iii) how to discriminate between the different star formation scenarios.
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