论文标题

开放群集二进制文件中潮汐循环的综合贝叶斯建模第一部分:M 35,NGC 6819,NGC 188

Comprehensive Bayesian Modeling of Tidal Circularization in Open Cluster Binaries part I: M 35, NGC 6819, NGC 188

论文作者

Penev, Kaloyan M., Schussler, Joshua A.

论文摘要

长期以来,潮汐摩擦会随着时间的流逝而循环循环二进制恒星的轨道。在这项研究中,我们使用观察到的唯一恒星种群中轨道偏心率的分布来探测潮汐耗散。与以前的研究相反,我们纳入了其他分析中经常忽略的许多物理效应,对潮汐,详细的单个系统(代替人口统计)提供了更一般的描述,并说明了所有观察不确定性。目的是提供可靠的测量潮汐耗散的性能,该特性由数据完全支持,正确地解释了不同的耗散,从而分别影响了每个对象上的每个潮汐,并随着恒星的内部结构而演变。我们在三个开放簇中的短期二进制二进制中提取潮汐耗散的高精度测量。我们发现,主序列上的潮汐质量因子落在$ 5.7 <\ log_ {10} q_ \ star'<6 $ 3至7.5天之间的范围内。相比之下,在150 Myr旧M 35群集中观察到的循环化要求预先序列的星星更耗散:$ q_ \ star'<4 \ 4 \ times10^4 $。我们测试了潮汐耗散的频率依赖性,发现在3至7.5天之间的潮汐周期(如果存在依赖性)中,则是主要序列恒星的亚线性。此外,通过使用更完整的物理模型进行进化,并考虑到每个系统的特定属性,我们可以减轻所分析的开放群集中先前观察到的循环化的紧张局势。

Tidal friction has long been recognized to circularize the orbits of binary stars over time. In this study, we use the observed distribution of orbital eccentricities in populations of binary stars to probe tidal dissipation. In contrast to previous studies, we incorporate a host of physical effects often neglected in other analyses, provide a much more general description of tides, model individual systems in detail (in lieu of population statistics), and account for all observational uncertainties. The goal is to provide a reliable measurement of the properties of tidal dissipation that is fully supported by the data, properly accounts for different dissipation affecting each tidal wave on each object separately, and evolves with the internal structure of the stars. We extract high precision measurements of tidal dissipation in short period binaries of Sun-like stars in three open clusters. We find that the tidal quality factor on the main sequence falls in the range $5.7 < \log_{10}Q_\star' < 6$ for tidal periods between 3 and 7.5 days. In contrast, the observed circularization in the 150 Myr old M 35 cluster requires that pre-main sequence stars are much more dissipative: $Q_\star' < 4\times10^4$. We test for frequency dependence of the tidal dissipation, finding that for tidal periods between 3 and 7.5 days, if a dependence exists, it is sub-linear for main-sequence stars. Furthermore, by using a more complete physical model for the evolution, and by accounting for the particular properties of each system, we alleviate previously observed tensions in the circularization in the open clusters analyzed.

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