期刊
SPACE SCIENCE REVIEWS
卷 212, 期 3-4, 页码 1271-1314出版社
SPRINGER
DOI: 10.1007/s11214-017-0411-3
关键词
Interplanetary coronal mass ejections; Interplanetary shocks; Space weather; Solar wind; Magnetic storms; Magnetosphere
资金
- Recruitment Program of Global Experts of China
- NSFC [41374173]
- Specialized Research Fund for State Key Laboratories of China
- Academy of Finland [1267087]
- UH three-year grant project [490162]
- HELCATS project [400931]
- European Research Council (ERC) under the European Union's Horizon research and innovation programme [SolMAG 724391]
Interplanetary Coronal Mass Ejections (ICMEs), their possible shocks and sheaths, and co-rotating interaction regions (CIRs) are the primary large-scale heliospheric structures driving geospace disturbances at the Earth. CIRs are followed by a faster stream where Alfvenic fluctuations may drive prolonged high-latitude activity. In this paper we highlight that these structures have all different origins, solar wind conditions and as a consequence, different geomagnetic responses. We discuss general solar wind properties of sheaths, ICMEs (in particular those showing the flux rope signatures), CIRs and fast streams and how they affect their solar wind coupling efficiency and the resulting magnetospheric activity. We show that there are two different solar wind driving modes: (1) Sheath-like with turbulent magnetic fields, and large Alfven Mach (MA) numbers and dynamic pressure, and (2) flux rope-like with smoothly varying magnetic field direction, and lower MA numbers and dynamic pressure. We also summarize the key properties of interplanetary shocks for space weather and how they depend on solar cycle and the driver.
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