The bulk of available stellar activity observations is frequently checked for the manifestation of signs in comparison with the known characteristic of solar magnetic modulation. The problem is that stellar activity records are usually an order of magnitude shorter than available observations of solar activity variation. Therefore, the resolved time scales of stellar activity are insufficient to decide reliably that a cyclic variation for a particular star is similar to the well-known 11-yr sunspot cycles. As a result, recent studies report several stars with double or multiple cycles which serve to challenge the underlying theoretical understanding. This is why a consistent method to separate 'true' cycles from stochastic variations is required. In this paper, we suggest that a conservative method, based on the best practice of wavelet analysis previously applied to the study of solar activity, for studying and interpreting the longest available stellar activity record - photometric monitoring of V833 Tau for more than 100 years. We find that the observed variations of V833 Tau with timescales of 2-50 yr should be comparable with the known quasi-periodic solar mid-term variations, whereas the true cycle of V833 Tau, if it exists, should be of about a century or even longer. We argue that this conclusion does not contradict the expectations from stellar dynamo theory.

中文翻译：

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V833 Tau长期活性的小波分析

与已知的太阳磁调制特性相比，大量可用的恒星活动观测结果经常被检查是否有迹象显示。问题是恒星活动记录通常比现有的太阳活动变化观测短一个数量级。因此，已解析的恒星活动时间尺度不足以可靠地确定特定恒星的周期性变化与众所周知的 11 年太阳黑子周期相似。因此，最近的研究报告了几颗具有双重或多重周期的恒星，这对潜在的理论理解提出了挑战。这就是为什么需要一种一致的方法来将“真实”周期与随机变化分开的原因。在本文中，我们建议采用一种保守的方法，基于之前应用于太阳活动研究的小波分析的最佳实践，用于研究和解释最长的可用恒星活动记录 - V833 Tau 100 多年的光度监测。我们发现观测到的 V833 Tau 在 2-50 年的时间尺度上的变化应该与已知的准周期性太阳中期变化相当，而 V833 Tau 的真实周期（如果存在）应该是大约一个世纪或甚至更长。我们认为这个结论与恒星发电机理论的预期并不矛盾。我们发现观测到的 V833 Tau 在 2-50 年的时间尺度上的变化应该与已知的准周期性太阳中期变化相当，而 V833 Tau 的真实周期（如果存在）应该是大约一个世纪或甚至更长。我们认为这个结论与恒星发电机理论的预期并不矛盾。我们发现观测到的 V833 Tau 在 2-50 年的时间尺度上的变化应该与已知的准周期性太阳中期变化相当，而 V833 Tau 的真实周期（如果存在）应该是大约一个世纪或甚至更长。我们认为这个结论与恒星发电机理论的预期并不矛盾。