Solar wind turbulence: Connections with energetic particles

被引：34

作者：

Oughton, Sean ^{[1
]}

Engelbrecht, N. Eugene ^{[2
]}

机构：

[1] Univ Waikato, Dept Math & Stat, Hamilton 3240, New Zealand

[2] North West Univ, Ctr Space Res, ZA-2522 Potchefstroom, South Africa

来源：

NEW ASTRONOMY | 2021年 / 83卷

关键词：

Solar wind; Turbulence; Transport; Cosmic rays; Waves; Magnetohydrodynamics; HELIOSPHERIC MAGNETIC-FIELD; GUIDING CENTER THEORY; RAY DIFFUSION TENSOR; GALACTIC COSMIC-RAYS; MEAN FREE-PATH; MAGNETOHYDRODYNAMIC TURBULENCE; PERPENDICULAR DIFFUSION; CHARGED-PARTICLES; MHD TURBULENCE; ALFVENIC FLUCTUATIONS;

D O I：

10.1016/j.newast.2020.101507

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

For the solar wind, a wealth of observational evidence indicates that turbulence is an important dynamical process for velocity (v), magnetic (b), and other related fluctuations at MHD (fluid) scales. Here we review such observations and turbulence features, including discussion of when wave or turbulence descriptions can (or cannot) explain the observations. The relevance of properties of MHD turbulence to the acceleration and transport of energetic particles is emphasized. A summary of different classes of models for solar wind fluctuations is presented, followed by reviews of transport models for (i) solar wind fluctuations and (ii) cosmic rays. In connection with cosmic ray transport models, recent developments in terms of cosmic ray transport coefficients, as well as their application in cosmic ray modulation models, are discussed in detail.

引用

页数：20

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