Recent progress in astrophysical plasma turbulence from solar wind observations
Recent progress in astrophysical plasma turbulence from solar wind observations
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DOI：
10.1017/s0022377816001124
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发表时间：
2016-11
影响因子：
2.5
通讯作者：
C. Chen
中科院分区：
文献类型：
--
作者：
C. Chen
本文总结了一些最近的进展，已在了解天体物理等离子体湍流的太阳风，从现场航天器的观测。在大尺度上，湍流主要是Alfvénic的，临界平衡，剩余能量和三维结构的测量进行了讨论，沿着与最近的强Alfvénic湍流模型进行比较。在这些尺度上，百分之几的能量也在压缩波动，它们的性质，各向异性和关系的Alfvénic组件描述。在小规模的动力学范围内，低于离子gyroscale，湍流成为主要动力学Alfvén的性质，和测量的光谱，各向异性和湍流的讨论相对于最近的级联模型。剩下的主要问题之一是如何耗散的湍流能量，和一些最近的工作在这个问题上，除了未来的空间任务，这将有助于回答这个问题，简要讨论。
This paper summarises some of the recent progress that has been made in understanding astrophysical plasma turbulence in the solar wind, from in situ spacecraft observations. At large scales, where the turbulence is predominantly Alfvénic, measurements of critical balance, residual energy and three-dimensional structure are discussed, along with comparison to recent models of strong Alfvénic turbulence. At these scales, a few per cent of the energy is also in compressive fluctuations, and their nature, anisotropy and relation to the Alfvénic component is described. In the small-scale kinetic range, below the ion gyroscale, the turbulence becomes predominantly kinetic Alfvén in nature, and measurements of the spectra, anisotropy and intermittency of this turbulence are discussed with respect to recent cascade models. One of the major remaining questions is how the turbulent energy is dissipated, and some recent work on this question, in addition to future space missions which will help to answer it, are briefly discussed.