Mirror mode structures in the solar wind at 0.72 AU

被引：52

作者：

Zhang, T. L. ^{[1
,2
]}

Baumjohann, W. ^{[1
]}

Russell, C. T. ^{[3
]}

Jian, L. K. ^{[3
]}

Wang, C. ^{[2
]}

Cao, J. B. ^{[4
]}

Balikhin, M. ^{[5
]}

Blanco-Cano, X. ^{[6
]}

Delva, M. ^{[1
]}

Volwerk, M. ^{[1
]}

机构：

[1] Austrian Acad Sci, Space Res Inst, A-8042 Graz, Austria

[2] Chinese Acad Sci, State Key Lab Space Weather, Beijing 100080, Peoples R China

[3] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90095 USA

[4] Beihang Univ, Sch Astronaut, Beijing 100083, Peoples R China

[5] Univ Sheffield, Dept Automat Control & Syst Engn, Sheffield S1 4DU, S Yorkshire, England

[6] Univ Nacl Autonoma Mexico, Inst Geophys, Mexico City 04510, DF, Mexico

来源：

JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS | 2009年 / 114卷

基金：

美国国家航空航天局;

关键词：

MAGNETIC HOLES; PLASMA; FIELD;

D O I：

10.1029/2009JA014103

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Magnetic holes in the solar wind with little or no directional change across the magnetic depression are related to mirror mode structures. Recently, Zhang et al. (2008) determined the characteristic size and shape of such mirror mode structures in the solar wind at 0.72 AU. They found that the mirror mode structure in the solar wind is quite elongated along the field direction. In this report, we examine the size and shape of isolated magnetic holes and train of holes, separately. We find that the isolated holes are slightly smaller in width and more elongated than the multiple holes. This observation suggests a particular evolutionary history of mirror mode structures in the solar wind in which multiple holes coalesce with time into isolated structures more elongated parallel to the magnetic field.

引用

页数：5

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