Abstract

This work is devoted to the study of properties of spectra of turbulent solar wind fluctuations in plasma compression regions, such as CIR (the plasma compression regions in front of high-speed streams from coronal holes) and SHEATH (the compression regions in front of interplanetary manifestations of coronal mass ejections EJECTA and magnetic clouds MC). The spectra of ion flux fluctuations, on both magnetohydrodynamic and ion-kinetic scales, are considered on the basis of data from the BMSW spectrometer on the SPEKTR-R spacecraft with a high (up to 31 ms) time resolution. The comparison of turbulent characteristics in the plasma compression regions and in the undisturbed solar wind is carried out both on a separate example and using extensive statistical material. It is shown in the paper that the turbulent cascade characteristics on the kinetic interval can significantly change in the plasma compression regions, and the signatures of a change in the main processes that determine the energy dissipation are revealed in them, which may cause increased heating in the regions under consideration.

中文翻译：

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等离子体压缩区太阳湍流特征

摘要

这项工作致力于研究等离子压缩区域（例如CIR（日冕孔高速流之前的等离子压缩区域）和SHEATH（行星际前面的压缩区域）等等离子体压缩区域中湍流太阳风波动的光谱特性。日冕物质抛射EJECTA和磁云MC的表现）。基于来自SPEKTR-R上BMSW光谱仪的数据，考虑了磁流体动力学和离子动力学尺度上离子通量波动的光谱具有高（高达31 ms）时间分辨率的航天器。在一个单独的例子中，并使用大量的统计资料，对等离子压缩区域和不受干扰的太阳风中的湍流特性进行了比较。本文表明，动力学间隔上的湍流级联特性会在等离子压缩区域发生显着变化，并在其中揭示了确定能量耗散的主要过程的变化特征，这可能会导致加热过程中热量的增加。正在考虑的区域。