Interferometry of $ε$ Aurigae: Characterization of the asymmetric eclipsing disk
Brian Kloppenborg, Robert Stencel, John D. Monnier, Gail Schaefer, Fabien Baron, Chris Tycner, Robert T. Zavala, Donald Hutter, Ming Zhao, Xiao Che, Theo ten Br… 展开作者
Brian Kloppenborg, Robert Stencel, John D. Monnier, Gail Schaefer, Fabien Baron, Chris Tycner, Robert T. Zavala, Donald Hutter, Ming Zhao, Xiao Che, Theo ten Brummelaar, Chris Farrington, Robert Parks, Hal McAlister, Judit Sturmann, Laszlo Sturmann, P. J. Sallave-Goldfinger, Nils Turner, Ettoree Pedretti, Nathalie Thureau
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105 pages, 57 figures. This is an author-created, un-copyedited version of an article accepted for publication in Astrophysical Journal Supplement Series. IOP Publishing Ltd is not responsible for any errors or omissions in this version of the manuscript or any version derived from it
We report on a total of 106 nights of optical interferometric observations of the $ε$ Aurigae system taken during the last 14 years by four beam combiners at three different interferometric facilities. This long sequence of data provides an ideal assessment of the system prior to, during, and after the recent 2009-2011 eclipse. We have reconstructed model-independent images from the 10 in-eclipse epochs which show that a disk-like object is indeed responsible for the eclipse. Using new 3D, time-dependent modeling software, we derive the properties of the F-star (diameter, limb darkening), determine previously unknown orbital elements ($Ω$, $i$), and access the global structures of the optically thick portion of the eclipsing disk using both geometric models and approximations of astrophysically relevant density distributions. These models may be useful in future hydrodynamical modeling of the system. Lastly, we address several outstanding research questions including mid-eclipse brightening, possible shrinking of the F-type primary, and any warps or sub-features within the disk.
High cadence measurement of neutral sodium and potassium absorption during the 2009-2011 eclipse of epsilon Aurigae
本文介绍了利用小型望远镜网在日食期间对御夫座进行分光观测的结果。光谱的分辨率为0.35至0.65厘米，涵盖了2008年至2012年，日食期间的典型间隔为4天。本文特别介绍了K I 7699、Na D和Mg II 4481等谱线的变异。KI 7699的吸收在日食开始前3个月开始增加，到2012年3月调查结束时，亮度已经恢复到正常的日食外水平7个月后，还没有恢复到日食前的水平。食星对KI 7699谱线的贡献被分离出来，数据显示在进入和离开期间，过量吸收以一系列的步骤增加和减少。这被解释为日食天体内部结构的指示。在食时，F星被Na D波长的食星完全遮蔽。F星的径向速度和在任何给定时间F星前面的食物质的平均和最大径向速度已经被分离出来，并在整个日食过程中被跟踪。在日食外的F星RV中看到的准周期变化在日食期间继续存在。希望这些结果可以用于约束系统及其组件的拟议模型。
Spectroscopic study of the late B-type eclipsing binary system AR Aurigae A and B: Towards clarifying the differences in atmospheric parameters and chemical abundances
