Binary Information from Open Clusters Using SEDS (BINOCS) Project: The Dynamical Evolution of the Binary Populations in Cluster Environments
Binary Information from Open Clusters Using SEDS (BINOCS) Project: The Dynamical Evolution of the Binary Populations in Cluster Environments
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使用 SEDS 来自开放星团的二进制信息 (BINOCS) 项目：星团环境中二进制总体的动态演化
DOI：
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发表时间：
2015
期刊：
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通讯作者：
B. Thompson
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文献类型：
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作者：
P. Frinchaboy;B. Thompson
摘要对星团内部动力学的研究主要是通过n体模拟来进行的。N-Body模拟的主要输入之一是双星的频率和质量分布，目前受限于从场双星推导出的关系。然而，要真正理解星团环境是如何演变的，需要来自星团内部的二进制数据，包括质量。迄今为止，关于星团中主、次双星质量的详细信息还很有限。目前可用的主要技术是径向速度测量，但深度有限。使用先前基于两波段光度法的研究，可能会覆盖不同的质量范围，对观察到的双星群产生潜在的差异解释。我们引入了一种新的二进制检测方法，即使用SEDs的开放簇二进制信息（BINOCS），该方法覆盖了改善簇n -体模拟输入和比较所需的宽质量范围。利用新观测到的年龄范围不同的关键疏散星团的多波长光度表（0.3 - 8微米），我们可以证明BINOCS方法通过与现有的基于rv的研究相比较，可以准确地确定未解析星团双星的二元成分质量。利用这种方法，我们展示了5个原型星团中0.4 - 2.5太阳质量的双星的动态演化结果，跨度为30 Myr到3.5 Gyr，以及双星种群如何作为质量的函数演化。
Abstract Studying the internal dynamics of stellar clusters is conducted primarily through N-Body simulations. One of the major inputs into N-Body simulations is the binary star frequency and mass distribution, which is currently constrained by relations derived from field binary stars. However to truly understand how clustered environments evolve, binary data from within star clusters is needed including masses. Detailed information on binaries masses, primary and secondary, in star clusters has been limited to date. The primary technique currently available has been radial velocity surveys that are limited in depth. Using previous two-band photometry-based studies that may cover different mass ranges produce potentially discrepant interpretations of the observed binary population. We introduce a new binary detection method, Binary INformation from Open Clusters Using SEDs (BINOCS) that covers the wide mass range needed to improve cluster N-body simulation inputs and comparisons. Using newly-observed multi-wavelength photometric catalogs (0.3 - 8 microns) of the key open clusters with a range of ages, we can show that the BINOCS method determines accurate binary component masses for unresolved cluster binaries through comparison to available RV-based studies. Using this method, we present results on the dynamical evolution of binaries from 0.4 - 2.5 solar masses within five prototypical clusters, spaning 30 Myr to 3.5 Gyr, and how the binary populations evolve as a function of mass.