arXiv 1105.01072011-05astro-ph.SR

在2009-2011年日食之前和期间，食双星御夫座的光谱和光度分析

Spectral and photometric analysis of the eclipsing binary epsilon Aurigae prior to and during the 2009-2011 eclipse

Pavel Chadima, Petr Harmanec, Philip D. Bennett, Brian Kloppenborg, Robert Stencel, Stevenson Yang, Hrvoje Bozic, Miroslav Slechta, Lenka Kotkova, Marek Wolf, P… 展开作者

Pavel Chadima, Petr Harmanec, Philip D. Bennett, Brian Kloppenborg, Robert Stencel, Stevenson Yang, Hrvoje Bozic, Miroslav Slechta, Lenka Kotkova, Marek Wolf, Petr Skoda, Viktor Votruba, Jeff L. Hopkins, Christian Buil, Davor Sudar

备注：: accepted for publication in A&A (April 5, 2011)
发表信息：: 2011A&A...530A.146C
DOI：: 10.1051/0004-6361/201116739

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摘要：

在1994年至2010年期间获得的一系列353个红色电子光谱，以及2010年日食的171个UBV光度观测，被分析，以更好地了解食双星eps Aur。主要结果如下。(1)我们试图通过解开eps Aur双星的观测光谱来恢复伴星的光谱，但失败了，但是我们能够解开大地线的光谱，并获得F型主星的平均光谱。然后将后者与合成光谱的网格进行比较，得到一些合理的T（eff）和log（g）值，但没有发现相当好的匹配，然而，我们得出结论，观察到的光谱是低重力恒星的光谱。(2)我们研究了过去16年来复杂的H-α线剖面的变化，特别强调了2009-2011年的日食期间，通过从观测到的光谱中减去平均日食H-α剖面（径向速度适当偏移）。我们发现，围绕着看不见的伴星的黑暗圆盘有一个扩展的“大气层”，它通过对F星投射的蓝移和红移的H-α“壳”反射来表现自己。值得注意的是，H-α壳层线首次出现在日食第一次接触前三年，当时系统距离最大距离不远。(3)几个强大的，未混合的谱线，以及UBV测光径向速度和中心强度的分析表明，这些观测显示出明显的多周期变化在日食。66.21的主周期是所有观测量所共有的，但这些变量之间的相移不同。这一结果有力地支持了我们先前的建议，即在日食期间看到的光度变化是F星固有的，因此，应该放弃由于盘中有一个洞而导致中心增亮的想法。

英文摘要：

A series of 353 red electronic spectra obtained between 1994 and 2010, and of 171 UBV photometric observations of the 2010 eclipse, were analyzed in an effort to better understand the eclipsing binary eps Aur. The main results follow. (1) We attempted to recover a spectrum of the companion by disentangling the observed spectra of the eps Aur binary failed, but we were able to disentangle the spectrum of telluric lines and obtain a mean spectrum of the F-type primary star. The latter was then compared to a grid of synthetic spectra for a number of plausible values of T(eff) and log(g), but a reasonably good match was not found. However, we conclude that the observed spectrum is that of a low-gravity star. (2) We examined changes in the complex H-alpha line profiles over the past 16 years, with particular emphasis on the 2009-2011 eclipse period, by subtracting a mean out-of-eclipse H-alpha profile (appropriately shifted in radial velocity) from the observed spectra. We find that the dark disk around the unseen companion has an extended 'atmosphere' that manifests itself via blueshifted and redshifted H-alpha 'shell' absorptions seen projected against the F star. Significantly, the H-alpha shell line first appeared three years before first contact of the optical eclipse when the system was not far past maximum separation. (3) Analyses of radial velocities and central intensities of several strong, unblended spectral lines, as well as UBV photometry, demonstrated that these observables showed apparent multiperiodic variability during eclipse. The dominant period of 66.21 was common to all the observables, but with different phase shifts between these variables. This result strongly supports our earlier suggestion that the photometric variability seen during eclipse is intrinsic to the F star, and therefore, the idea of a central brightening due to a hole in the disk should be abandoned.

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