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首页> 外文期刊>Journal of Geophysical Research, A. Space Physics: JGR >Kronian Magnetospheric Reconnection Statistics Across Cassini’s Lifetime
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Kronian Magnetospheric Reconnection Statistics Across Cassini’s Lifetime

机译：Kronian磁性层的重新连接数据在卡西尼号的一生

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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 R_S. This research introduces prediction equations to estimate the distribution of duration of plasmoid passage over the spacecraft (N=300Δt~(-1.3), bin width = 1 min) and north-south field deflection (N=52ΔB_θ~(2.1) , 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 s~(-1) on average, which is comparable with the magnetospheric mass loading from Enceladus (8-250 kg s~(-1)).
机译：磁场重联是一个基本的物理在行星不但的过程,在这个过程中,等离子体太阳风之间可以交换和一个行星磁层,材料断开连接,最终失去的磁气圈。行星磁尾会导致释放的等离子粒团downtail dipolarizationsplanetward x轴。产品包括变位特征磁场的南北分量可以检测到现场飞船。这些签名发现了眼睛,半自动算法,以及最近的机器学习(ML)方法。分析Kronian最全面的目录磁性层的重新连接创建签名通过ML方法改进的理解磁性层的进化。没有准恒定磁尾的位置在70 R_S x轴存在。介绍了预测方程来估计分布的等离子粒团一段时间宇宙飞船(N = 300Δt ~(-1.3),宽度= 1分钟),南北场偏转(N = 52ΔB_θ~(2.1),本宽度= 0.25元)的预期来确定轨道飞船一年的观察。研究发现一个当地时间的不对称重新连接标识,偏好对于dusk-side dawn-side。偏爱Vasyliunas风格重新连接土星Dungey风格。分布,土星的重联率磁尾可以估计为3.22重新连接每天的事件,产生最大的质量从等离子粒团损失44.87公斤s ~ (1)一般来说,这是可比的磁性层的质量负载从土卫二(8 - 250公斤(s ~(1))。

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