Solar wind origins in coronal holes and in the quiet Sun

被引：17
|
作者：
He, J. -S. [1 ,2 ]
Tu, C. -Y. [1 ]
Tian, H. [1 ,2 ]
Marsch, E. [2 ]
机构：
[1] Peking Univ, Dept Geophys, Beijing 100871, Peoples R China
[2] Max Planck Inst Sonnensyst Forsch, D-37191 Katlenburg Lindau, Germany
来源：
ADVANCES IN SPACE RESEARCH | 2010年 / 45卷 / 02期
基金：
中国国家自然科学基金; 中国博士后科学基金;
关键词：
Solar wind origin; Coronal hole; Quiet Sun; INTRANETWORK MAGNETIC ELEMENTS; TRANSITION-REGION; ACTIVE REGIONS; PLASMA FLOWS; ALFVEN WAVES; ACCELERATION; FIELDS; LINES; LOOPS; RECONNECTION;
D O I：
10.1016/j.asr.2009.07.020
中图分类号：
V [航空、航天];
学科分类号：
08 ; 0825 ;
摘要：
Coronal hole (CH) and the quiet Suit (QS) are considered to account for sources of fast and slow solar wind streams, respectively. The differences between the solar wind streams flowing out from the CH and the QS are thought to be related with different plasma generation and acceleration mechanisms in the respective source regions. Here we review recent studies on the solar wind origin in the CH and the QS, compare the possible flow geometries and magnetic structures in these two kinds of solar regions, and summarize the physics associated with two different origin scenarios. (C) 2009 COSPAR. Published by Elsevier Ltd. All rights reserved.
引用
收藏
页码：303 / 309
页数：7
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