In this paper, we present four sets of photometric V RI light curves, and several LAMOST low and medium resolution spectra of contact binary CC Com. We revised the orbital parameters by simultaneously combining with previously published radial velocity measurements using the Wilson-Devinney program. We used light curves at different observational times to obtain the starspot parameters. The values of the starspot radius are variable in short- and long-term scales, and their longitudes are stable. We updated the orbital period change of CC Com, and analyzed the periodic variation. The period of CC Com decreases at a rate of 4.66 (0.20) 10⁻¹¹ d yr⁻¹, which may be due to mass transfer from the secondary component to the primary component. The oscillation of its orbital period with a period of 17.18(0.08) years and amplitude of 0.0018(1) d may be caused by the light time effect (LITE) via a third body of 0.06 M _⊙ dwarf or magnetic activity cycle. Furthermore, we obtained one optical spectrum from the LAMOST survey, which gives the spectral type of CC Com as K72V. Strong emissions exist in the Hα, and Ca ii H&K lines in the observed spectrum, indicating strong chromospheric activity on CC Com. In the 12 LAMOST medium-resolution spectra, the EWs of Hα line are variable along the phase and time, which may be a plage or flare event.

在本文中，我们提出了四组光度V RI光曲线，以及接触二元 CC Com 的几个 LAMOST 低分辨率和中分辨率光谱。我们通过同时结合之前发布的使用 Wilson-Devinney 程序的径向速度测量值来修改轨道参数。我们使用不同观测时间的光变曲线来获得星斑参数。星斑半径的值在短期和长期尺度上是可变的，它们的经度是稳定的。我们更新了CC Com的轨道周期变化，并分析了周期变化。CC Com 的周期以 4.66 (0.20) 10 ^-11 d yr ^{-1的速度减少}，这可能是由于从次要组分到主要组分的质量转移。其轨道周期为17.18(0.08)年、振幅为0.0018(1) d的振荡，可能是由0.06 M⊙矮星或磁活动周期的第三天体的光时效应(LITE)引起 的_。此外，我们从 LAMOST 调查中获得了一个光谱，它给出了 CC Com 的光谱类型为 K72V。观测光谱中的 H α和 Ca ii H&K 谱线中存在强发射，表明 CC Com 上有强烈的色球活动。在12张LAMOST中分辨率光谱中，Hα线的EW沿相位和时间变化，可能是斑纹或耀斑事件。