Stawarz J E, Muñoz P A, Bessho N, Bandyopadhyay R, Nakamura T K M, Eriksson S, Graham D B, Büchner J, Chasapis A, Drake J F, Shay M A, Ergun R E, Hasegawa H, Khotyaintsev Yu V, Swisdak M, Wilder F D
Department of Mathematics, Physics, and Electrical Engineering, Northumbria University, Ellison Building, Newcastle upon Tyne, NE1 8ST UK.
Center for Astronomy and Astrophysics, Technical University Berlin, 10623 Berlin, Germany.
Space Sci Rev. 2024;220(8):90. doi: 10.1007/s11214-024-01124-8. Epub 2024 Nov 25.
Alongside magnetic reconnection, turbulence is another fundamental nonlinear plasma phenomenon that plays a key role in energy transport and conversion in space and astrophysical plasmas. From a numerical, theoretical, and observational point of view there is a long history of exploring the interplay between these two phenomena in space plasma environments; however, recent high-resolution, multi-spacecraft observations have ushered in a new era of understanding this complex topic. The interplay between reconnection and turbulence is both complex and multifaceted, and can be viewed through a number of different interrelated lenses - including turbulence acting to generate current sheets that undergo magnetic reconnection (), magnetic reconnection driving turbulent dynamics in an environment () or acting as an intermediate step in the excitation of turbulence, and the random diffusive/dispersive nature of the magnetic field lines embedded in turbulent fluctuations enabling so-called . In this paper, we review the current state of knowledge on these different facets of the interplay between turbulence and reconnection in the context of collisionless plasmas, such as those found in many near-Earth astrophysical environments, from a theoretical, numerical, and observational perspective. Particular focus is given to several key regions in Earth's magnetosphere - namely, Earth's magnetosheath, magnetotail, and Kelvin-Helmholtz vortices on the magnetopause flanks - where NASA's mission has been providing new insights into the topic.
与磁重联一样，湍流是另一种基本的非线性等离子体现象，在空间和天体物理等离子体的能量传输和转换中起着关键作用。从数值、理论和观测的角度来看，在空间等离子体环境中探索这两种现象之间的相互作用有着悠久的历史；然而，最近的高分辨率、多航天器观测开启了理解这个复杂主题的新时代。重联与湍流之间的相互作用既复杂又多方面，可以通过许多不同的相互关联的视角来审视——包括湍流作用产生经历磁重联的电流片（）、磁重联在某一环境中驱动湍流动力学（）或作为湍流激发的中间步骤，以及嵌入湍流涨落中的磁力线的随机扩散/色散性质促成所谓的 。在本文中，我们从理论、数值和观测的角度，回顾了在无碰撞等离子体（如在许多近地天体物理环境中发现的等离子体）背景下，关于湍流与重联之间相互作用的这些不同方面的当前知识状态。特别关注了地球磁层中的几个关键区域——即地球的磁鞘、磁尾以及磁层顶侧翼的开尔文 - 亥姆霍兹涡旋——美国国家航空航天局的 任务一直在这些区域为该主题提供新的见解。
