arXiv 2104.079342021-04astro-ph.SR

用Kepler/K2鉴定行星状星云的双星

Binary Central Stars of Planetary Nebulae Identified With Kepler/K2

George H. Jacoby, Todd C. Hillwig, David Jones, Kayla Martin, Orsola De Marco, Matthias Kronberger, Jonathan L. Hurowitz, Alison F. Crocker, Josh Dey

备注：: 21 pages, 11 figures, 4 tables. Accepted for publication in MNRAS
DOI：: 10.1093/mnras/stab2045

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摘要：

本文利用{ \it Kepler/K2}资料识别了34颗可能的行星状星云中心双星，其中7颗有日食现象。其中29个是新发现。另外两个CS更复杂的变化也提出。我们检查了所有“可能的”，“可能的”和“真正的”PNe在每个{ \it开普勒/K2}活动（0至19）的光变曲线，以确定CS的变化，可能表明一个二进制CS。对于运动0，2，7，15和16，我们发现6个可能的或确认的变量中的21个PNE。然而，我们的主要工作集中在第11次战役中，目标是一个包含大约183个PNe的银河系凸起区域，其中我们确定了30个候选的可变CS。这些变星的周期从2.3~h到30~d不等，根据我们的分析，它们中的大多数可能是近距离双星系统。我们目前的时期和初步分类（食，双退化，或照射系统）的基础上可能的二进制光曲线形状。从我们的204个目标PNe的总样本中，由于星等限制的不完整性进行了校正，我们计算出PN中心恒星的二进制分数为20.7%，对于所有观测到的PNe，或者23.5%，如果我们将样本限制为“真正的”PNe。然而，这些分数几乎肯定是较低的限制，由于大的角度大小的\emph{Kepler}像素，这导致降低灵敏度检测变化，主要是由于稀释和噪音，从星云和邻近的恒星。我们讨论的二进制人口的CS根据这些结果的一部分，总已知的样本的密切二进制CS。

英文摘要：

We present the identification of 34 likely binary central stars (CSs) of planetary nebulae (PNe) from {\it Kepler/K2} data, seven of which show eclipses. Of these, 29 are new discoveries. Two additional CSs with more complicated variability are also presented. We examined the light curves of all `possible', `likely' and `true' PNe in every {\it Kepler/K2} campaign (0 through 19) to identify CS variability that may indicate a binary CS. For Campaigns 0, 2, 7, 15, and 16 we find 6 likely or confirmed variables among 21 PNe. Our primary effort, though, was focused on Campaign 11 which targeted a Galactic bulge field containing approximately 183 PNe, in which we identified 30 candidate variable CSs. The periods of these variables range from 2.3~h to 30~d, and based on our analysis, most are likely to be close binary star systems. We present periods and preliminary classifications (eclipsing, double degenerate, or irradiated systems) for the likely binaries based on light curve shape. From our total sample of 204 target PNe, with a correction for incompleteness due to magnitude limits, we calculate a binary fraction of PN central stars to be 20.7 percent for all the observed PNe, or 23.5 percent if we limit our sample only to `true' PNe. However these fractions are almost certainly lower limits due to the large angular size of the \emph{Kepler} pixels, which leads to reduced sensitivity in detecting variability, primarily as a result of dilution and noise from the nebula and neighbouring stars. We discuss the binary population of CSs based on these results as part of the total known sample of close binary CSs.

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