Abstract—According to the exact positions and proper motions of the three components of the star ADS48 from Gaia DR2, their parallax and radial velocities for the epoch 2015.5 the instantaneous relative positions and motions of the components were determined. Only from the Gaia DR2 observations, the family of orbits of the AB pair was calculated by the method of apparent motion parameters, from which those that best agree with the Pulkovo data were selected. Comparison with the first observations of the 19th century made it possible to independently estimate the sum of the masses of the components in the range 1.15 < M_{A + B} < 1.4 M_⊙. The orbits of the outer pair were calculated: with a minimum period of 79 × 10³ years and the most probable one—about 3 × 10⁵ years. It is concluded that the system is stable for the most probable value of the relative− radial velocity ∆V_r = 0.7 km s^–1 and may be unstable near the boundaries of the possible velocity difference. A detailed analysis of homogeneous Pulkovo observations revealed a disturbance with a period of 11 years. It is shown that this disturbance is associated not with a star, but with a periodic climatic process that changes the observation conditions. Comparison of instantaneous and average relative motion does not exclude the presence of a planetary mass satellite in one of the components.

摘要—根据盖亚DR2恒星ADS48的三个分量的精确位置和正确运动，确定了它们在2015.5时代的视差和径向速度，确定了这些分量的瞬时相对位置和运动。仅从Gaia DR2观测中，通过视在运动参数的方法计算出AB对的轨道族，然后从中选择最符合Pulkovo数据的轨道。与19世纪的最初观察结果进行比较，就有可能独立地估计范围1内的组件的总和。15 <M _{A + B} < 1 。4中号_⊙。计算了外层对的轨道：最短周期为79×10 ³年，最可能的周期约为3×10 ⁵年。结论是，该系统对于相对径向速度∆ V _r = 0的最可能值是稳定的。7公里s ^–1并且在可能的速度差的边界附近可能不稳定。对均匀的普尔科沃观测资料的详细分析显示，扰动持续了11年。结果表明，这种扰动与恒星无关，而与改变观测条件的周期性气候过程有关。瞬时相对运动和平均相对运动的比较不排除在组件之一中存在行星质量卫星。