A NOVEL METHOD FOR IDENTIFYING EXOPLANETARY RINGS
A NOVEL METHOD FOR IDENTIFYING EXOPLANETARY RINGS
复制标题
识别系外行星环的新方法
DOI：
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发表时间：
2015
期刊：
影响因子：
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通讯作者：
Jaime A. Alvarado
中科院分区：
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作者：
J. Zuluaga;D. Kipping;Mario Sucerquia;Jaime A. Alvarado
太阳系外行星环的发现是系外行星研究的下一个突破。以前的研究探讨了检测与现在和未来的光度灵敏度exorings寻求异常偏差的标准过境光曲线拟合的残差，在1000？Kronian环的ppm。在这项工作中，我们探讨了两个更大的观测结果的驱逐：（1）过境深度的显着增加，可能会导致错误的分类环行星候选人作为假阳性和/或低估行星密度;以及（2）所谓的“光环”效应，一种新的小行星密度剖面效应，通过比较由光变曲线导出的恒星密度与用独立方法测量的恒星密度（例如，asteroseismology）。虽然这些方法不能提供对驱逐的明确检测，但我们表明，这些效应的大幅值，加上其相对简单的分析描述，使它们非常适合大规模调查，以识别值得更详细调查的候选环形行星。此外，这些方法有助于合奏分析，试图揭示人口的环状行星的证据。我们详细描述的方法，开发的基本形式主义，并测试它在环和过境配置的参数空间。我们讨论的前景，使用这种方法的第一个系统的搜索系外行星环的开普勒数据库，并提供了一个基本的计算代码来实现它。
The discovery of rings around extrasolar planets (“exorings”) is one of the next breakthroughs in exoplanetary research. Previous studies have explored the feasibility of detecting exorings with present and future photometric sensitivities by seeking anomalous deviations in the residuals of a standard transit light curve fit, at the level of ≃ 100 ?> ppm for Kronian rings. In this work, we explore two much larger observational consequences of exorings: (1) the significant increase in transit depth that may lead to the misclassification of ringed planetary candidates as false-positives and/or the underestimation of planetary density; and (2) the so-called “photo-ring” effect, a new asterodensity profiling effect, revealed by a comparison of the light curve derived stellar density to that measured with independent methods (e.g., asteroseismology). While these methods do not provide an unambiguous detection of exorings, we show that the large amplitude of these effects, combined with their relatively simple analytic description, makes them highly suited to large-scale surveys to identify candidate ringed planets worthy of more detailed investigation. Moreover, these methods lend themselves to ensemble analyses seeking to uncover evidence of a population of ringed planets. We describe the method in detail, develop the basic underlying formalism, and test it in the parameter space of rings and transit configuration. We discuss the prospects of using this method for the first systematic search of exoplanetary rings in the Kepler database and provide a basic computational code for implementing it.