Tracing heliospheric structures to their solar origin
Tracing heliospheric structures to their solar origin
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DOI：
10.1063/1.4943857
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发表时间：
2014-12
期刊：
影响因子：
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通讯作者：
R. Wimmer–Schweingruber;D. Hassler
中科院分区：
文献类型：
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作者：
R. Wimmer–Schweingruber;D. Hassler
太阳风的组成是太阳风/日冕起源的极好的示踪剂。我们总结了太阳风从太阳扩展到日光层时影响其组成的各种过程。当太阳风离开混合良好的光球层时，在高度演化的色球/过渡区，太阳风根据第一电离势(FIP)或第一电离时间(FIT)进行分馏。当它在日冕的动态环境中移动时，它的电荷状态会进一步改变。
The composition of the solar wind serves as an excellent tracer of the solar/coronal origin of the solar wind. We summarize various processes which affect the composition of the solar wind as it expands from the Sun into the heliosphere. As it leaves the well-mixed photosphere, the solar wind is fractionated according to First Ionization Potential (FIP) or First Ionization Time (FIT) in the highly evolving chromosphere/transition region. Its charge states are further modified as it moves through the dynamic environment of the corona.