Radial Evolution of Magnetic Field Fluctuations in an Interplanetary Coronal Mass Ejection Sheath

被引：24

作者：

Good, S. W. ^{[1
]}

Ala-Lahti, M. ^{[1
]}

Palmerio, E. ^{[1
,2
]}

Kilpua, E. K. J. ^{[1
]}

Osmane, A. ^{[1
]}

机构：

[1] Univ Helsinki, Dept Phys, Helsinki, Finland

[2] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA

来源：

ASTROPHYSICAL JOURNAL | 2020年 / 893卷 / 02期

基金：

芬兰科学院; 欧洲研究理事会;

关键词：

Solar wind; Interplanetary magnetic fields; Interplanetary turbulence; SOLAR-WIND TURBULENCE; DRIVEN; WAVES; EARTH;

D O I：

10.3847/1538-4357/ab7fa2

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

The sheaths of compressed solar wind that precede interplanetary coronal mass ejections (ICMEs) commonly display large-amplitude magnetic field fluctuations. As ICMEs propagate radially from the Sun, the properties of these fluctuations may evolve significantly. We have analyzed magnetic field fluctuations in an ICME sheath observed by MESSENGER at 0.47 au and subsequently by STEREO-B at 1.08 au while the spacecraft were close to radial alignment. Radial changes in fluctuation amplitude, compressibility, inertial-range spectral slope, permutation entropy, Jensen-Shannon complexity, and planar structuring are characterized. These changes are discussed in relation to the evolving turbulent properties of the upstream solar wind, the shock bounding the front of the sheath changing from a quasi-parallel to quasi-perpendicular geometry, and the development of complex structures in the sheath plasma.

引用

页数：10

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