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| 1 | Statistical properties of kinetic-scale magnetic holes in terrestrial space显示文摘Kinetic-scale magnetic holes(KSMHs)are structures characterized by a significant magnetic depression with a length scale on the order of the proton gyroradius.These structures have been investigated in recent studies in near-Earth space,and found to be closely related to energy conversion and particle acceleration,wave-particle interactions,magnetic reconnection,and turbulence at the kineticscale.However,there are still several major issues of the KSMHs that need further study—including(a)the source of these structures(locally generated in near-Earth space,or carried by the solar wind),(b)the environmental conditions leading to their generation,and(c)their spatio-temporal characteristics.In this study,KSMHs in near-Earth space are investigated statistically using data from the Magnetospheric Multiscale mission.Approximately 200,000 events were observed from September 2015 to March 2020.Occurrence rates of such structures in the solar wind,magnetosheath,and magnetotail were obtained.We find that KSMHs occur in the magnetosheath at rates far above their occurrence in the solar wind.This indicates that most of the structures are generated locally in the magnetosheath,rather than advected with the solar wind.Moreover,KSMHs occur in the downstream region of the quasi-parallel shock at rates significantly higher than in the downstream region of the quasi-perpendicular shock,indicating a relationship with the turbulent plasma environment.Close to the magnetopause,we find that the depths of KSMHs decrease as their temporal-scale increases.We also find that the spatial-scales of the KSMHs near the subsolar magnetosheath are smaller than those in the flanks.Furthermore,their global distribution shows a significant dawn-dusk asymmetry(duskside dominating)in the magnetotail. | ShuTao Yao ZongShun Yue QuanQi Shi Alexander William Degeling HuiShan Fu AnMin Tian Hui Zhang Andrew Vu RuiLong Guo ZhongHua Yao Ji Liu Qiu-Gang Zong XuZhi Zhou JingHuan Li WenYa Li HongQiao Hu YangYang Liu WeiJie Sun | 2021 | Earth and Planetary Physics2021，5，1： | 1 |
| 2 | 无碰撞磁场重联中的磁岛显示文摘在以下两个方面回顾了磁岛在无碰撞磁场重联中的作用:磁能到等离子体动能和热能的快速转化以及高能量电子的产生.重联的X点附近的电流片可能被拉伸并导致撕裂模不稳定性,并形成相互作用的次级磁岛.这种非稳态的磁场重联图像可以维持长时间的高重联率,进而有效地耗散磁能.电子可在磁岛内通过费米和betatron机制加速,也可在X点附近通过重联电场加速.磁岛间的相互作用可进一步加速电子.这些加速过程可导致高能量电子的幂律谱分布. | 陆全明 王荣生 黄楷 王水 | 2020 | 中国科学技术大学学报2020，50，9： | 0 |
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