Magnetic reconnection is a fundamental physical process in planetary magnetospheres, in which plasma can be exchanged between the solar wind and a planetary magnetosphere, and material can be disconnected and ultimately lost from a magnetosphere. Magnetic reconnection in a planetary magnetotail can result in the release of plasmoids downtail and dipolarizations planetward of an x-line. The signatures of these products include characteristic deflections in the north-south component of the magnetic field which can be detected by in-situ spacecraft. These signatures have been identified by eye, semi-automated algorithms, and recently machine learning (ML) methods. Here, we apply statistical analysis to the most thorough catalog of Kronian magnetospheric reconnection signatures created through ML methods to improve understanding of magnetospheric evolution. This research concludes that no quasi-steady position of the magnetotail x-line exists within 70 . This research introduces prediction equations to estimate the distribution of duration of plasmoid passage over the spacecraft (, bin width = 1 min) and north-south field deflection (, bin width = 0.25 nT) expected to be identified by an orbiting spacecraft across a year of observations. Furthermore, this research finds a local time asymmetry for reconnection identifications, with a preference for dusk-side over dawn-side. This may indicate a preference for Vasyliunas style reconnection over Dungey style for Saturn. Finally, through these distributions, the reconnection rate of Saturn’s magnetotail can be estimated as 3.22 reconnection events per day, with a resulting maximum mass loss from plasmoids of 44.87 kg on average, which is comparable with the magnetospheric mass loading from Enceladus (8–250 kg ).

中文翻译：

---

卡西尼号整个生命周期的克罗尼亚磁层重联统计

磁重联是行星磁层中的一个基本物理过程，其中等离子体可以在太阳风和行星磁层之间交换，物质可以断开并最终从磁层中丢失。行星磁尾中的磁重联会导致等离子团向下释放和 x 线行星的偶极化。这些产品的特征包括磁场南北分量的特征偏转，可以由原位航天器检测到。这些签名已通过眼睛、半自动算法和最近的机器学习 (ML) 方法进行识别。这里，我们将统计分析应用于通过 ML 方法创建的最全面的克朗磁层重联特征目录，以提高对磁层演化的理解。本研究得出结论，磁尾x线在70°以内不存在准稳态位置。. 本研究引入了预测方程来估计轨道航天器预计将在一年内识别出的等离子体团通过航天器的持续时间分布 ( , bin 宽度 = 1 分钟) 和南北场偏转 ( , bin 宽度 = 0.25 nT)的观察。此外，这项研究发现了重新连接识别的本地时间不对称性，优先于黄昏侧而不是黎明侧。这可能表明土星更喜欢 Vasyliunas 风格的重新连接而不是 Dungey 风格的重新连接。最后，通过这些分布，土星磁尾的重联率可以估计为每天 3.22 次重联事件，由此产生的等离子体团的最大质量损失为 44.87 kg平均而言，这与土卫二（8-250 kg ）的磁层质量负载相当。