The relation between the transit depths of KIC 12557548b and the stellar rotation period
The relation between the transit depths of KIC 12557548b and the stellar rotation period
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KIC 12557548b的凌日深度与恒星自转周期的关系
DOI：
10.1093/mnras/stv297
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发表时间：
2014
影响因子：
4.8
通讯作者：
A. Levine
中科院分区：
文献类型：
--
作者：
B. Croll;S. Rappaport;A. Levine
川原和他的合作者分析了候选解体的水星质量行星KIC 12557548b的凌日，并提出凌日深度与恒星自转的阶段有关。我们分析了KIC12557548b的凌日深度，并确认在黑子主星自转周期的凌日深度确实存在一个强健的、具有统计意义的信号。这个信号在开普勒数据的前半部分更加突出，并不是由于旋转的光斑信号泄漏到我们对凌日深度的测量中，也不是由于未掩星的恒星黑子。我们调查了这样的假设，即这个信号可能是由于恒星上的一个活跃区域，发射了增强的紫外线或X射线辐射，导致行星质量损失率增加；我们确认，这种情况可能会导致KIC12557548b凌日深度的调制，以及足够小的凌日计时变化，以至于它们可能在开普勒数据中检测不到。KIC12557548b的凌日深度受恒星自转相位的调制，我们倾向于解释这一事实是，凌日行星遮蔽了这颗高度聚集的恒星上的恒星黑子；这样的情况可能会引起与已观测到的一样大的凌日深度变化，并造成足够小的凌日时间变化，以至于它们可以与开普勒数据相一致。
Kawahara and collaborators analyzed the transits of the candidate disintegrating Mercury-mass planet KIC 12557548b and suggested that the transit depths were correlated with the phase of the stellar rotation. We analyze the transit depths of KIC 12557548b and confirm that there is indeed a robust, statistically significant signal in the transit depths at the rotation period of the spotted host star. This signal is more prominent in the first-half of the Kepler data, and is not due to leakage of the rotating spot signal into our measurement of the transit depths, or due to unocculted starspots. We investigate the suggestion that this signal could be due to an active region on the star, emitting enhanced ultraviolet or X-ray radiation leading to an increased mass loss rate of the planet; we confirm that such a scenario could cause both modulation of the transit depths of KIC 12557548b, and small enough transit-timing variations that they might not be detected in the Kepler data. Our preferred explanation for the fact that the transit depths of KIC 12557548b are modulated with the stellar rotation phase is that the candidate transiting planet is occulting starspots on this highly spotted star; such a scenario could cause transit depth variations as large as have been observed, and cause transit-timing variations small enough that they are arguably consistent with the Kepler data.
影响因子：
4.8
作者：
S. Barros;G. Boué;G. Boué;G. Boué;N. P. Gibson;D. Pollacco;A. Santerne;F. Keenan;I. Skillen;R. Street
通讯作者：
S. Barros;G. Boué;G. Boué;G. Boué;N. P. Gibson;D. Pollacco;A. Santerne;F. Keenan;I. Skillen;R. Street
影响因子：
6.5
作者：
S. Czesla;K. Huber;U. Wolter;S. Schröter;J. Schmitt
通讯作者：
S. Czesla;K. Huber;U. Wolter;S. Schröter;J. Schmitt