Observational research on Mercury's magnetosphere
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摘要: 水星磁层无辐射带、电离层、等离子层，大气层明显消失，只有微弱的外逸层. 由于磁层尺度小，行星内核感应效应较为明显. 行星空间环境显著区别于地球. “信使”号卫星对水星磁层的观测研究丰富了对水星空间环境的认识和理解. 本文主要从磁层尺度及变化性、磁场重联及磁通量绳的形成、典型磁层动力学活动过程、磁层行星重离子时空变化、极端太阳事件下磁层响应特征等方面对水星磁层“信使”号观测研究进展进行简要总结. 并对BepiColombo卫星探测进行相关问题研究展望.Abstract: Mercury's miniature magnetosphere has no radiation belts, ionosphere, plasmasphere and atmosphere, only a weak exosphere. The induction effect of the planet's very large iron core is obvious. These result in a significant different space environment from that of the Earth. Observations of Mercury's magnetosphere by the MESSENGER spacecraft have enriched the knowledge and understanding of Mercury's space environment. Here, recent advances in Mercury's magnetosphere observational research are briefly summarized, from the aspects of magnetospheric scale and variability, magnetic reconnection and the formation of magnetic flux ropes, typical magnetospheric dynamic activity process, spatial and temporal variations of magnetospheric planetary heavy ions, magnetospheric response characteristics to the extreme solar events. Some related topics for the future exploration of BepiColombo mission are prospected.
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Key words:
- Mercury /
- magnetosphere /
- MESSENGER
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图 2 水星磁尾磁重联区观测.（a）～（c）为穿越磁尾电流片的概况；（d）～（i）为穿越电流片中心重联扩散区的详细数据.（a）、（b）为磁场强度及在MSM坐标系下三分量；（c）离子能谱数据；（d）～（g）磁场强度及在局地电流片LMN坐标系下三分量；（h）NS仪器探测高能电子（>20～40 keV）计数率. 根据BN磁场结构及变化特征，离子扩散区可以划分为5个不同特征的时间段：T1～T5，分别对应于右示意图（修改自Zhong et al., 2018）
Figure 2. MESSENGER observations of an active reconnection site in Mercury's magnetotail. Panels (a)～(c) show an overview of the current sheet crossing. Panels (d)～(i) show a subset of the data near the diffusion region. (a),(b) The magnetic field magnitude and its three components in the LMN coordinates. (c) Spectrogram of the ion differential energy flux. (d)～(g) The magnetic field magnitude and its three components. (h) Count rate of energetic electrons detected from the NS instrument with 1 s resolution in its burst mode. The diffusion region crossing is divided into five short subintervals, T1～T5. Right: Schematic of the rapidly evolving reconnection process in Mercury's magnetotail (modified from Zhong et al., 2018)
图 3 水星空间大尺度磁通量绳结构形成过程示意图.（a）众多离子尺度磁通量绳相互作用、多步骤合并形成FTEs;（b）近磁尾和远磁尾重联形成等离子体团结构；（c）极端太阳风条件下磁尾电流片撕裂模不稳定性形成多重联线及离子尺度磁岛链，众多磁岛合并形成大尺度磁通量绳，并周期性释放典型的水星磁层能量输入、输出过程（修改自Zhong et al., 2019, 2020a, 2020c）
Figure 3. Schematic of macroscale flux rope structures formation in Mercury's space. (a) Macroscale FTEs at Mercury's dayside magnetopause; (b) Giant plasmoid formed and trapped between two widely separated reconnection sites in Mercury's magnetotail; (c) Multiple X-line reconnection in Mercury's magnetotail. (top) Formation of ion-scale flux ropes and the occurrence of multiple X-line reconnection in the elongated tail current sheet. (bottom) Formation of a large-scale flux rope through the interaction and coalescence of many of ion-scale flux ropes and their tailward ejection（modified from Zhong et al., 2019, 2020a, 2020c）
图 4 （a）水星磁层亚暴膨胀相期间阿尔芬波及压缩波的形成示意图（修改自Sun et al., 2015a). （b）水星磁尾亚暴电流楔形成的直接观测结果示意图（修改自Poh et al., 2017a)
Figure 4. (a) A schematic to illustrate the Alfvénic and compressional waves generated during the substorm expansion phase in Mercury's magnetotail (modified from Sun et al., 2015a). (b) Schematic illustrations of asymmetries in Mercury's current sheet. Left: the formation of a substorm current wedge in the near-Mercury region. Right: current sheet structure in the postmidnight and premidnight views (modified from Poh et al., 2017a)
图 5 不同磁场大小下水星磁层顶K-H波多尺度特征. 夜侧磁层顶K-H波的频率和局地Na+回旋频率接近，由于磁场大小的不同，频率可以小于（a）、等于（b）或大于（c）日测K-H波频率（修改自Gershman et al., 2015）
Figure 5. Illustration of K-H wave growth along Mercury's magnetopause for increasing magnetic field given a constant vortex speed. Toward the tail, where the Na+ is expected to dominate the plasma mass density, the observed frequency of K-H waves (blue spacecraft) matches that of the Na+ gyrofrequency, which can be (a) less than, (b) equal to, or (c) greater than that observed on the dayside (red spacecraft) (modified from Gershman et al., 2015)
图 6 （a）极尖区观测到的Na+形成机制.（左）太阳风离子溅射和光电离；（右）磁层顶附近或太阳风区域外逸层中性原子电离，被太阳风“拾起”进入极尖区和磁层（修改自Raines et al., 2014）.（b）THEMIS遥感探测外逸层典型Na分布模式.（上）日侧低纬单峰模式;（下）中纬地区双峰模式（修改自Mangano et al., 2015）
Figure 6. (a) Two possible sources for Na+ ions in the cusp: (left) Na+ ions are generated in the cusp, both by solar wind impact and photoionization, and are accelerated by processes there. (right) Neutral Na atoms are ionized near the magnetopause and swept into the cusp (modified from Raines et al., 2014). (b) Examples of the 8 recurrent Na emission patterns identified in the Mercury's exosphere. Top: equatorial Peak. Bottom: two peaks in middle latitude (modified from Mangano et al., 2015)
图 7 左：少数极端情况下卫星轨道未穿越向阳侧磁层事例.（a）～（d）磁场强度及其三分量；（e）磁场天顶角（红）和方位角（蓝）；（f）质子能谱，磁场在（g）X-Z 平面和（h）X-Y平面的投影，以及弓激波（BS）和磁层顶（MP）观测位置与平均磁层顶模型（虚曲线）的比较（修改自Zhong et al., 2015a）. 右：向阳侧磁层消失事件观测结果示意图（修改自Slavin et al., 2019）
Figure 7. Left: Example of MESSENGER missed the dayside magnetosphere. (a)～(d) Magnetic field intensity and its three components; (e) magnetic field zenith and azimuthal angles; (f) spectrogram of proton flux, and the MESSENGER orbit and the vector plots of the magnetic field in the (g) noon-midnight and (h) equatorial planes relative to Mercury's surface (circle) and the average magnetopause from the model (dashed linesh) (modified from Zhong et al., 2015a) . Right: Illustration of the primary features of the disappearing dayside magnetosphere events (modified from Slavin et al., 2019)
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