Recently research advances on the polar cap patches
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摘要: 极盖区等离子体云块是一种经常出现在极区电离层F层的高密度块状结构，其电子密度一般是背景电子密度的两倍及以上，水平尺度约为100～1000 km. 极盖区等离子体云块的产生及演化过程可以示踪磁层-电离层/热层耦合过程中的能量及动量传输过程. 同时，这种电子密度不均匀体（尤其是其边沿区域）对跨极盖区的无线电波传播具有很强的干扰，经常影响无线电通讯导航定位等应用. 因而，极盖区等离子体云块研究不仅是空间物理领域的热点问题，而且也是空间天气监测及准确预报等应用的重要基础. 本文简述了近十年来极盖区等离子体云块的研究进展，主要内容包括：概括了极盖区等离子体云块几种可能的形成机制；提出了极盖区冷/热等离子体云块的分类研究；统计了极盖区等离子体云块的时空分布特征及其对外部条件的依赖性；追踪了极盖区等离子体云块的完整演化过程；最后，讨论了极盖区等离子体云块引起的离子上行现象及电离层闪烁效应.
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关键词:
- 极盖区冷/热等离子体云块 /
- 发生概率 /
- 演化过程 /
- 离子上行 /
- 电离层闪烁
Abstract: The polar cap patch is a common ionospheric structure. It often appears in the F region of the ionosphere over the polar caps; these patches are usually characterized by electron densities that can be even twice greater than that of the surrounding area. Untangling the formation and evolution of the polar cap patch can unveil the transportation of energy and momentum through magnetosphere-ionosphere-thermosphere couplings. However, owing to their wide horizontal reach (~100～1000 km), these high electron density structures greatly obstruct radio wave propagation over the polar cap, particularly at their edges, seriously impeding efforts tied to communication, navigation, and positioning. Therefore, the study of polar cap patches is not only of significance within space physics but also of great value within the context of space weather monitoring and prediction. In this paper, recent progress in polar cap patch research is summarily reviewed. The focus of our review includes the possible mechanisms underlying the formation of the dominant dayside reconnection; the recently proposed sunward return flows, likely produced by the nightside reconnection or other processes; and the newly defined patch-polar cap hot patch and its dependencies on various factors (e.g., solar & geomagnetic activities, local plasma transport, and particle precipitation). We will also delve into patch occurrences, as they relate to spatiotemporal dynamics as well as the interplanetary magnetic field conditions. We will also comprehensively review the evolutionary process tied to the Dungey convection cycle, as it moves from the dayside to the nightside and finally as it exits the polar caps, initially modulated by the pulsed nightside reconnection and then sunward transportation by the return flow. Lastly, we will detail the effects of ion upflow and ionospheric scintillation associated with the polar cap patch. For each subject, we will provide a detailed account of progress that has been made and its corresponding prospects. -
图 1 （a-f） 速度流携带着日侧高密度等离子体进入极隙区和极盖区，进而形成舌状电离区，然后被日侧磁层顶磁重联调制的脉冲式爆发速度流“切割”成等离子体云块的形成过程概念图. MLT：磁地方时； ESR：欧洲非相干散射雷达；VHF：甚高频雷达（修改自Zhang et al., 2013b）
Figure 1. (a-f) Schematic explaining how an elongated channel of high plasma density enters the cusp and polar cap region, forms a tongue of ionization (TOI), and then is segmented into patches by transient changes in flow channels generated by pulsed dayside magnetopause reconnection (modified from Zhang et al., 2013b)
图 2 2012年1月30日，DMSP卫星（F16）观测到的极盖区冷/热等离子体云块事件对比图（修改自Zhang et al., 2017）
Figure 2. A detailed comparisons of characteristics of polar cap cold/hot patches observed by DMSP F16 satellite on Jan 30, 2012 (modified from Zhang et al., 2017)
图 3 2005—2018年期间，极盖区等离子体云块月发生数量与太阳黑子数（左列）、AE指数（右列）的相关性. （a, b）表示极盖区冷等离子体云块；（c, d）为热等离子体云块（修改自Zhang et al., 2021）
Figure 3. Comparison between sunspot number (left)/AE index (right) and number of patches in each month from 2005 to 2018. (a, b) For cold patches; (c, d) For hot patches (modified from Zhang et al., 2021)
图 4 基于Swarm A（蓝色）和Swarm B（红色）观测数据，等离子体云块发生率统计结果. （a, b）分别为北/南半球. 黑色水平实线标出冬季时间，青色/橙色竖虚线分别给出当地冬季/夏季至点（修改自Spicher et al., 2017）
Figure 4. Patch occurrence rate observed by Swarm A (blue) and Swarm B (red). (a) The Northern Hemisphere, and (b) the Southern Hemisphere. The black horizontal lines highlight local wintertime taken between both equinoxes, and the vertical cyan and orange dashed lines mark local winter and summer solstices, respectively (modified from Spicher et al., 2017)
图 5 利用2013年Madrigal GPS TEC观测，在年积日与UT坐标下，不均匀体与背景TEC值的比值（修改自David et al., 2016）
Figure 5. Based on the Madrigal GPS TEC maps for 2013, the patch-(tongue-)-to-background ratio is plotted as a function of day of year and universal time (modified from David et al., 2016)
图 6 Swarm卫星观测的极盖区等离子体云块发生率空间分布特征. 这里采用MLat-MLT坐标系. （a, c）来自Swarm A；（b, d）来自Swarm B. （a, b）为北半球（NH）；（c, d）为南半球（SH）（修改自Spicher et al., 2017）
Figure 6. Spatial distribution of polar cap patches provided by Swarm A/B satellites under MLat/MLT coordinate. The left/right panels, respectively, from Swarm A/B. (a, b) The Northern Hemisphere; (c, d) The Southern Hemisphere (modified from Spicher et al., 2017)
图 7 不同IMF By/Bz分量条件下，极盖区等离子体云块发生率在MLT上的分布（修改自Jin et al., 2019）
Figure 7. MLT distributions of patch occurrences during different IMF By/Bz conditions (modified from Jin et al., 2019)
图 8 2011年9月26日17:55—21:45 UT期间，地磁坐标系下TEC map叠加对流结构的时间序列图. 日侧在上方，晨侧在右边. 黑色同心圆为等势线，表征对流结构. 黑色虚线为100 km高度处晨昏线. 蓝色圆圈及椭圆追踪极盖区等离子体云块的演化过程（修改自Zhang et al., 2013a）
Figure 8. Extracts from a full series of 2D maps of TEC and ionospheric convection on a geomagnetic latitude/MLT during 17:55—21:45 UT on Sep 11, 2011. Noon is on top; dawn is on the left. The black concentric circles suggest the convection cell. The black dashed lines represent the day–night terminator at the altitude of 100 km. The blue circles and ellipses highlight the full evolution of a polar cap patch (modified from Zhang et al., 2013a)
图 9 在亚暴恢复相，当IMF Bz分量从强负值跳转至~0 nT时，极区电离层响应示意图. （a） IMF Bz、By分量时间序列值；（b, d）分别为当IMF Bz分量为强南向时日侧磁重联及极区电离层概念图；（c, e）分别为当IMF Bz分量突变为~0 nT时日侧磁重联及极区电离层概念图. 在图（b）和（c）中，红/蓝箭头线表示磁鞘/磁层的磁力线，洋红色实线代表日侧磁层顶重联区域. 在图（d）和（e）中，带箭头的红色同心圆表征对流结构，黄色圆圈表示开-闭磁力线边界，其中日侧蓝色线段及夜侧红色线段分别表示磁重联发生位置，白色亮斑表征极盖区等离子体云块沿对流结构的演化过程（修改自Zhang et al., 2016a）
Figure 9. Schematic of the response of the northern polar ionosphere to the IMF Bz component turning from strongly southward to varying around 0 nT during a substorm recovery phase. (a) The IMF By and Bz components; (b) and (d) morphology of dayside magnetic reconnection and the polar ionosphere for strong southward and weak dawnward IMF; and (c) and (e) morphology of dayside magnetic reconnection and polar ionosphere for weak southward and strong duskward IMF. In (b) and (c), red/blue lines (with arrow) show magnetic field lines in magnetosheath/magnetosphere, and magenta solid lines show the reconnection X-line at dayside magnetopause. In (d) and (e), the red concentric with arrows suggest the convection streamlines, the yellow circle suggests the open–close boundary, at which the blue sector for dayside and red sector for nightside, respectively, indicate the magnetic reconnection region; the white patches outline the full evolution of the polar cap patch along the streamlines (modified from Zhang et al., 2016a)
图 10 （a） 在MLat/MLT坐标系下，DMSP F17的卫星观测叠加地面二维TEC map. 图中彩色粗线表征DMSP F17卫星轨迹，颜色表示O+密度；垂直于轨道的淡紫色线条表示水平速度；蓝色椭圆圈出极盖区等离子体云块. （b） 在南向IMF与正IMF By条件下，北半球极盖区等离子体云块伴随的离子上行概念图（修改自Zhang et al., 2016b; Zong et al., 2020）
Figure 10. (a) In-situ ion parameters by DMSP F17 superimposed on 2-D maps of median-filtered TEC on a MLat/MLT grid, and (b) schematic of the ionospheric upflow/outflow associated with polar cap patches above the Northern Hemisphere during a southward IMF with a positive IMF By component (modified from Zhang et al., 2016b; Zong et al., 2020)
图 11 离子上行发生率、上行速度及上行O+密度/通量分别与对流速度、太阳天顶角、太阳射电流量F10.7的依赖关系（修改自Ma et al., 2018b）
Figure 11. Dependence investigations of ion upflow occurrence and ion upflow speed and upflow O+ density/flux on parameters of convection and solar zenith angle (SZA) and F10.7 (modified from Ma et al., 2018b)
图 12 （a）全空天成像仪观测叠加地面接收机-NIMS卫星链路的穿越路径;（b）地面接收机观测的闪烁指数（修改自Coker et al., 2004）
Figure 12. (a) An all-sky image of F region patch with a NIMS satellite pass superimposed on it; (b) The related scintillation indices provided by the ground-based receiver (modified from Coker et al., 2004)
图 13 （a-d） 极盖区等离子体云块D南向运动进入极光椭圆（红色区域），叠加接收机观测的GPS卫星穿刺点位置；（e-h）各极盖区等离子体云块引起的电离层相位闪烁及TEC扰动的时间序列值（修改自Jin et al., 2014）
Figure 13. (a-d) The polar cap patch D moved southward and then entered into the auroral oval (red regions), superimposed with the IPPs of GPS satellites; (e-h) The corresponding time series of phase scintillations and TECs produced by 3 patches observed by the ground-based receiver from GPS satellites (modified from Jin et al., 2014)
图 14 GPS TEC叠加CHAIN广域电离层闪烁（灰色方块），两条黑色实线表征极光椭圆边界，（a-d）叠加幅度闪烁指数；（e-h）叠加相位闪烁指数，SED：暴时密度增强结构；TOI：舌状电离区（修改自Wang et al., 2016）
Figure 14. The GPS TEC maps combined with the ionospheric scintillations (represented by the grey squares), the two solid black curves highlight the auroral oval. (a-d) Projected the amplitude scintillation indices; (e-h) Superimposed the phase scintillations indices (modified from Wang et al., 2016)
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