University of Birmingham Asteroseismology of the solar analogs 16 Cyg A and B from Kepler observations-猫眼课题宝

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2012

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T. Metcalfe;W. Chaplin;T. Appourchaux;R. García;S. Basu;I. Brandao;O. Creevey;S. Deheuvels;G. Doğan;P. Eggenberger;C. Karoff;A. Miglio;D. Stello;M. Yıldız;Z. Celik;H. M. Antia;O. Benomar;R. Howe;C. Régulo;D. Salabert;T. Stahn;T. Bedding;G. Davies;Y. Elsworth;L. Gizon;S. Hekker;S. Mathur;B. Mosser;S. Bryson;M. Still;J. Christensen-Dalsgaard;R. Gilliland;S. Kawaler;H. Kjeldsen;K. Ibrahim;T. Klaus;J. Li

演化后的太阳型恒星 16 Cyg A 和 B 长期以来一直作为太阳类比进行研究，让我们得以一睹太阳的未来。双星系统的轨道周期太长，无法对恒星特性提供有意义的动力学约束，但星震学可以提供帮助，因为这些恒星是开普勒场中最亮的恒星之一。我们对开普勒太空望远镜对 16 Cyg A 和 B 进行的三个月几乎不间断的光度测量进行了分析。我们分别提取了两个分量的总共 46 和 41 个振荡频率，包括清晰检测到两颗恒星中的八极 ( l = 3) 模式。我们使用星震建模门户独立推导每颗恒星的属性，同时拟合各个振荡频率和其他观测约束。我们根据各种恒星演化代码和拟合方法生成的结果集合来评估系统不确定性。通过单独拟合每个组件而得出的最佳模型在不确定性范围内产生了共同年龄（t = 6 . 8 ± 0 . 4 Gyr）和初始成分（Z i = 0 . 024 ± 0 . 002，Y i = 0 . 25 ± 0 . 01），正如对双星系统组件的预期一样，增强了我们对星震技术可靠性的信心。最终可用的更长的数据集将允许未来研究差异旋转、对流区深度以及恒星活动周期引起的长期变化。

The evolved solar-type stars 16 Cyg A and B have long been studied as solar analogs, yielding a glimpse into the future of our own Sun. The orbital period of the binary system is too long to provide meaningful dynamical constraints on the stellar properties, but asteroseismology can help because the stars are among the brightest in the Kepler ﬁeld. We present an analysis of three months of nearly uninterrupted photometry of 16 Cyg A and B from the Kepler space telescope. We extract a total of 46 and 41 oscillation frequencies for the two components, respectively, including a clear detection of octupole ( l = 3) modes in both stars. We derive the properties of each star independently using the Asteroseismic Modeling Portal, ﬁtting the individual oscillation frequencies and other observational constraints simultaneously. We evaluate the systematic uncertainties from an ensemble of results generated by a variety of stellar evolution codes and ﬁtting methods. The optimal models derived by ﬁtting each component individually yield a common age ( t = 6 . 8 ± 0 . 4 Gyr) and initial composition ( Z i = 0 . 024 ± 0 . 002 , Y i = 0 . 25 ± 0 . 01) within the uncertainties, as expected for the components of a binary system, bolstering our conﬁdence in the reliability of asteroseismic techniques. The longer data sets that will ultimately become available will allow future studies of differential rotation, convection zone depths, and long-term changes due to stellar activity cycles.

University of Birmingham Asteroseismology of the solar analogs 16 Cyg A and B from Kepler observations

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