论文标题
迈出三个灾难变量的性质：LS CAM，V902 MON和SWIFT J0746.3-1608
A Step towards Unveiling the Nature of Three Cataclysmic Variables: LS Cam, V902 Mon, and SWIFT J0746.3-1608
论文作者
论文摘要
我们使用长基线的高基线光学光度数据（来自Transing Explanet Esperiplanet调查卫星（TESS）（TESS）（TESS），我们对三个灾难变量（CVS）进行了详细的时间分辨时间分析（CVS）。我们对LS CAM观测的分析暗示了$ 4.025 $ \ pm $ 0.007 d的超晶型期的存在，分别为$ \ sim $ 3.30 h和3.70 h，而负面和正上的超级人口周期分别为$ \ sims。这些结果可以解释为积聚盘与轨道运动的淋巴结和Apsidal进动的相互作用。对于其他两个来源，V902 Mon和Swift J0746.3-1608，我们发现了2387.0 $ \ pm $ \ pm $ 0.6 s和2409.5 $ \ pm $ 0.7 s的证据，在早期研究中找不到。我们在这项研究中提出的结果表明，在两个来源的整个观察期间，积聚模式的变化。对于V902 MON，还发现了（6.09 $ \ pm $ 0.60）$ \ times 10^{ - 10} $的明显轨道周期衍生物。此外，轨道频率的第二个谐波主导了Swift J0746.3-1608的功率谱，这暗示了次级恒星的椭圆形调制。目前的分析表明，LS CAM可能是一个超级凸起的简历，而V902 MON和SWIFT J0746.3-1608可能是可变的圆盘跨流量吸收中间极点。
We have carried out detailed time-resolved timing analyses of three cataclysmic variables (CVs) namely LS Cam, V902 Mon, and SWIFT J0746.3-1608, using the long-baseline, high-cadence optical photometric data from the Transiting Exoplanet Survey Satellite (TESS). Our analysis of LS Cam observations hints the presence of a superorbital period of $\sim$ 4.025$\pm$0.007 d along with negative and positive superhump periods of $\sim$ 3.30 h and 3.70 h, respectively. These results can be explained as an interaction of nodal and apsidal precession of the accretion disc with orbital motion. For the other two sources, V902 Mon and SWIFT J0746.3-1608, we have found evidence of a beat period of 2387.0$\pm$0.6 s and 2409.5$\pm$0.7 s, respectively, which were not found in earlier studies. Our results presented in this study indicate the change in the accretion mode during the entire observing period for both sources. For V902 Mon, an apparent orbital period derivative of (6.09 $\pm$ 0.60) $\times 10^{-10}$ was also found. Moreover, the second harmonic of orbital frequency dominates the power spectrum of SWIFT J0746.3-1608, suggestive of ellipsoidal modulation of the secondary star. Present analyses suggest that LS Cam could be a superhumping CV whereas V902 Mon and SWIFT J0746.3-1608 are likely to be variable disc-overflow accreting intermediate polars.
