Abstract—We present new results of the study of ET Dra—a star of the FK Com type—based on observations carried out at the Zvenigorod Observatory of the Institute of Astronomy of RAS with the help of the FRAM-ORM telescope of the La Palma observatory (Spain) and the broadband optical monitoring system Mini-MegaTORTORA, located on the territory of the SAO RAS. We have studied changes in the shape of the light curve caused by the rotational modulation of a star with spots on its surface and the long-term variability of the star’s brightness. An independent determination of the rotation period of \({{P}_{{{\text{phot}}}}}\) was carried out using all sets of observations available to us. The increase in the brightness of the star near HJD 2459044 during observations with the FRAM-ORM telescope in all three filters was interpreted by us as a stellar flare. Our flare energy estimates are \(2.8 \times {{10}^{{37}}}\), \(1.9 \times {{10}^{{37}}}\), and \(1.5 \times {{10}^{{37}}}\) erg in the \(B\), \(V\), and \(R\) wavelength ranges, respectively. Observations with a duration of more than 2200 days, carried out at the SAO RAS, opened up the possibility of analyzing the long-term brightness variability of ET Dra. Evidence was found for the existence of cycles lasting 580 days and 810 days (1.55 and 2.23 years, respectively).

摘要——我们基于拉帕尔马 FRAM-ORM 望远镜在 RAS 天文研究所 Zvenigorod 天文台进行的观测，展示了 FK Com 型恒星 ET Dra 研究的新结果天文台（西班牙）和位于 SAO RAS 领土上的宽带光学监测系统 Mini-MegaTORTORA。我们研究了表面有斑点的恒星旋转调制引起的光变曲线形状变化，以及恒星亮度的长期变化。\({{P}_{{{\text{phot}}}}}\)旋转周期的独立确定是使用我们可用的所有观察集进行的。在使用 FRAM-ORM 望远镜进行的所有三个滤光片观测期间，HJD 2459044 附近恒星亮度的增加被我们解释为恒星耀斑。我们的耀斑能量估计为\(2.8 \times {{10}^{{37}}}\)、\(1.9 \times {{10}^{{37}}}\)和\(1.5 \times { {10}^{{37}}}\)在\(B\)、\(V\)和\(R\)波长范围，分别。在 SAO RAS 进行的持续时间超过 2200 天的观测开启了分析 ET Dra 长期亮度变化的可能性。发现存在持续 580 天和 810 天（分别为 1.55 年和 2.23 年）的周期的证据。