论文标题
OAUNI天文光度法：2016年FO AQR的出色变异性
OAUNI astronomical photometry: Stellar variability of FO Aqr on 2016 low state
论文作者
论文摘要
这项工作报告了对中间极性灾难性变量恒星fo aqr的光度监测。这是正在进行的OAUNI恒星变异计划的一部分。大约有1200个单独的测量值（或$ \ sim $ 9小时的观测值）在五个晚上分发。观察时期与FO AQR的2016年亮度相吻合。高质量的光曲线明确检测到FO〜AQR的预期恒星变异性。使用周期图的分析以确定主要的两个已知周期，p $ _ {1} $〜= 〜20.380〜 $ \ pm $〜.003〜min和p $ _ {2} $〜= 〜11.076〜 $ \ $ \ pm $ 〜.001〜min。我们的完整五晚分析表明，p $ _ {1} $是旋转白色矮人期，比p $ _ {2} $（旋转和轨道时期之间的节拍期的一半）更为突出。然而，至少在一种情况下，单个光曲线显示出比发现反向模式的。它表明，在同一相间隔内具有重要变化的系统轨道阶段的依赖性。
This work reports a photometric monitoring of the intermediate polar cataclysmic variable star FO Aqr. This is part of the ongoing OAUNI stellar variability program. Around 1200 individual measurements (or $\sim$ 9 hrs of observations) were gathered distributed in five nights. The observation epoch was coincident with the 2016 low state brightness of FO Aqr. Good quality light curves detect unambiguously the expected stellar variability of FO~Aqr. The analysis using periodograms let to determine the main two known periods, P$_{1}$~=~20.380~$\pm$~.003~min and P$_{2}$~=~11.076~$\pm$~.001~min. Our full five-nights analysis shows that P$_{1}$, the spin white dwarf period, is more prominent than P$_{2}$, the one-half of the beat period between the spin and orbital periods. Nevertheless, individual light curves show than, at least in one case, a reverse pattern is found. It suggests a dependence of the beat period with the orbital phase of the system with important variations at the same phase interval.
