We develop a statistical test on the expected difference in age estimates of two coeval stars in detached double-lined eclipsing binary systems that are only caused by observational uncertainties. We focus on stars in the mass range [0.8; 1.6] Msun, and on stars in the main-sequence phase. The ages were obtained by means of the maximum-likelihood SCEPtER technique. The observational constraints used in the recovery procedure are stellar mass, radius, effective temperature, and metallicity [Fe/H]. We defined the statistic W computed as the ratio of the absolute difference of estimated ages for the two stars over the age of the older one. We determined the critical values of this statistics above which coevality can be rejected. The median expected difference in the reconstructed age between the coeval stars of a binary system -- caused alone by the observational uncertainties -- shows a strong dependence on the evolutionary stage. This ranges from about 20% for an evolved primary star to about 75% for a near ZAMS primary. The median difference also shows an increase with the mass of the primary star from 20% for 0.8 Msun stars to about 50% for 1.6 Msun stars. The reliability of these results was checked by repeating the process with a grid of stellar models computed by a different evolutionary code. We show that the W test is much more sensible to age differences in the binary system components than the alternative approach of comparing the confidence interval of the age of the two stars. We also found that the distribution of W is, for almost all the examined cases, well approximated by beta distributions. The proposed method improves upon the techniques that are commonly adopted for judging the coevality of an observed system. It also provides a result founded on reliable statistics that simultaneously accounts for all the observational uncertainties.
Discovery of a Highly Unequal-Mass Binary T Dwarf with Keck Laser Guide Star Adaptive Optics: A Coevality Test of Substellar Theoretical Models and Effective Temperatures
（节略）在野外棕矮星中，质量比高度不等的双星是很罕见的，已知的统计数据是q^（4.9+/-0.7）。然而，这样的系统可以测试的联合精度的演变和大气模型，在coevality的约束下（“等时线测试”）。我们使用目前已知的两个最极端的亚星双星，T1+T6 \eps Ind Bab双星和新发现的0.14”T2.0+T7.5双星，2 MASS 1209- 10 AB进行了这项测试。根据H-R图上各组分的位置，模型成功地表明这些系统是同时代的，内部年龄差分别为log（年龄）= 0.5{+0.4}{-0.3}和-0.8+/-1.3 dex。然而，从H-R图推导出的\eps Ind Bab的总质量（~80 Mjup）与报道的动力学质量不一致。这个问题，这是独立的假设年龄的系统，可以解释为一个~50-100 K的系统误差，在模型大气拟合;使两个质量测定一致导致推断年龄~6 Gyr的\eps Ind系统，比以前假设的。总的来说，这里研究的两个T矮星双星，以及最近在年龄和质量基准系统中T矮星的结果，在演化模型和/或模型大气中产生小（~100 K）误差的证据，但不是显着更大。最后，2 MASS 1209-10AB的二进制性质降低了其作为主要T3近红外光谱分型标准的实用性;我们建议SDSS 1206+28作为替代品。
Statistical structure and physical interpretation of the fillout factor distribution in contact binary stars
LUX, Observatoire de Paris, CNRS, PSL（巴黎天文台）；Astronomy Department, Raderon AI Lab., BC.（不列颠哥伦比亚大学天文学系雷德伦人工智能实验室）；Shandong Key Laboratory of Space Environment and Exploration Technology, Institute of Space Sciences, School of Space Science and Technology, Shandong University（山东大学空间科学与技术学院空间科学研究所山东省空间环境与探测技术重点实验室）；Binary Systems of South and North (BSN) Project（南北双星项目；独立研究者）；Independent Researcher（恰纳卡莱18马尔特大学理学院物理系）；Çanakkale Onsekiz Mart University, Faculty of Science, Department of Physics（恰纳卡莱18马尔特大学天体物理学研究中心乌鲁帕纳尔天文台）；Çanakkale Onsekiz Mart University, Astrophysics Research Center and Ulupnar Observatory（法提赫苏丹梅赫梅特基金会大学科学史系）；Fatih Sultan Mehmet Vakif University, Department of History of Science
Differential velocity cumulative distribution (DVCD): an efficient statistical method for binary-star analysis in large stellar catalogues using radial velocities
National Astronomical Observatories, Chinese Academy of Sciences（中国科学院国家天文台）；University of Chinese Academy of Sciences（中国科学院大学）
Statistical study for binary star evolution in dense embedded clusters
Helmholtz-Institut für Strahlen- und Kernphysik, Universität Bonn（波恩大学赫尔姆霍兹射线与核物理研究所）；Astronomical Institute, Faculty of Mathematics and Physics, Charles University（查理大学数学与物理学院天文研究所）
Millions of Main-Sequence Binary Stars from Gaia BP/RP Spectra
Max-Planck-Institut für Astronomie（马克斯·普朗克天文学研究所）；Department of Astronomy, The Ohio State University（俄亥俄州立大学天文学系）；Center for Cosmology and AstroParticle Physics (CCAPP), The Ohio State University（俄亥俄州立大学宇宙学与天体粒子物理中心）；Department of Astronomy, California Institute of Technology（加州理工学院天文学系）；Key Lab of Space Astronomy and Technology, National Astronomical Observatories（国家天文台空间天文与技术重点实验室）；Institute for Frontiers in Astronomy and Astrophysics of Beijing Normal University（北京师范大学天文与前沿科学研究院）；University of Chinese Academy of Sciences（中国科学院大学）；Zhejiang Lab（浙江实验室）
