论文标题
重新讨论黯然失色的二进制文件。纸IX。太阳能系统KIC 5359678
Rediscussion of eclipsing binaries. Paper IX. The solar-type system KIC 5359678
论文作者
论文摘要
KIC 5359678是一个6.231-D时期F型黯然失色的二进制系统，其组件恒星均显示出星点的活动。开普勒卫星长期以来在任务的整整四年期间都观察到了这一点。 Wang等人（2021）获得了两颗恒星的径向速度测量值，并分析了这些恒星以及开普勒数据以研究其斑点活动并测量其物理特性，但留下了几个问题。我们已经进行了独立的分析，并确定了恒星的质量（1.252 +/- 0.018和1.065 +/- 0.013 msun）和半径（1.449 +/- 0.012和1.048 +/- 0.017 rsun）。由于未知原因，我们发现系统的距离比Gaia EDR3的距离略短。我们还研究了应用于模型光曲线的数值集成的精度，以匹配开普勒观测值的1765-S采样节奏。我们发现，忽略这种时间涂抹会导致恒星的偏差半径测量值：对于初级涂抹4个sigma，而对于次要的恒星太小，而次要的恒星太小了。将模型光曲线的采样率加倍就足以消除大部分偏见，但是为了确切的结果，每个观察到的数据点至少需要五个样本。
KIC 5359678 is a 6.231-d period F-type eclipsing binary system whose component stars both show starspot activity. It was observed by the Kepler satellite in long cadence for the full four-year duration of the mission. Wang et al (2021) obtained radial velocity measurements of the two stars and analysed these plus the Kepler data to study their spot activity and measure their physical properties, but left several questions unanswered. We have performed an independent analysis and determined the masses (1.252 +/- 0.018 and 1.065 +/- 0.013 Msun) and radii (1.449 +/- 0.012 and 1.048 +/- 0.017 Rsun) of the stars to high precision. The distance we find to the system is slightly shorter than that from Gaia EDR3 for unknown reason(s). We also investigated the precision of the numerical integration applied to the model light curve to match the 1765-s sampling cadence of the Kepler observations. We found that ignoring this temporal smearing leads to biased radius measurements for the stars: that for the primary is too small by 4 sigma and that for the secondary is too large by 10 sigma. Doubling the sampling rate of the model light curve is sufficient to remove most of this bias, but for precise results a minimum of five samples per observed datapoint is required.
