AI 中文总结
该研究对赫瓦尔天文台53年的UBV测光进行精确归约与标准化，用新非线性方程及随时间变化的消光处理数据，将59颗Be星分类，给出各类别恒星百分比及相关变异性特征，为Be星变异性研究和模型测试提供了有价值数据集。
AI 中文摘要
发射线恒星Be在从几天到几十年的各种时间尺度上表现出光和颜色的变化。其演化必须通过精确校准且稳定的长期观测来约束。本文提供了对赫瓦尔天文台超过50年光电UBV观测的新归约。该独特数据集对TESS具有高度互补性。使用新的非线性归约方程及夜间随时间变化的消光，经约翰逊标准验证长期精度达0.008至0.016星等（1西格玛不确定度）。将59颗Be星按变异性模式分为五类，给出各类别恒星百分比，还发现样本中恒星常呈现多种模式，如LTE正向变异性比反向更常见等。观测提供了校准良好的数十年UBV光变曲线，为Be星变异性研究和模型测试提供了有价值数据集，对部分恒星持续监测很重要。
英文摘要
Emission-line stars classified as Be exhibit light and colour variability on various timescales, ranging from days to decades. Their evolution must be constrained by long-term observations that are accurately calibrated and stable. Here, we provide a new reduction of photoelectric UBV observations obtained at the Hvar observatory, spanning more than 50 years. This unique dataset is highly complementary to TESS. We used new, non-linear reduction equations, with temporally variable extinction over the course of the night, which allowed us to achieve long-term accuracy of 0.008 to 0.016 mag (1-sig uncertainty), as verified by the Johnson standards. We then classified 59 Be stars into five classes, based on their variability patterns; namely, long-term envelope (LTE), long-term cyclic (LTC), binarity (BIN), rapid low-amplitude (RLA), and long-term quiescence (LTQ). According to our observations, the percentages of stars in the individual classes are 44%, 24%, 25%, 66%, and 19%, respectively. The stars in the sample often exhibited more than one pattern. We confirm that the LTE-positive variability is more common than the inverse (20 vs 6); in addition, two stars exhibited both types (zeta Tau and V1294 Aql). According to our observations, the LTC variability and the LTE-positive variability are almost mutually exclusive. Among 26 binary systems, circular orbits are more common than eccentric ones (18 vs 8). As for the brightness variations between different quiescent phases, an increasing trend is less common than a decreasing one (4 vs 7), spanning from -6.5 to +6.0 mmag/yr. Our observations provide well-calibrated UBV light curves spanning several decades, offering a valuable dataset for investigations of Be-star variability and tests of various models, including the viscous decretion disc model. Continuous monitoring is important for beta Lyr, EW Lac, delta Sco, gamma Cas, and V1294 Aql.
Comments30 pages
Journal refAstronomy & Astrophysics, 712, A226 (2026)
