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ON THE SOLAR WIND ELEMENTAL COMPOSITION: CONSTRAINTS ON THE ORIGIN OF THE SOLAR WIND

机译：关于太阳风的元素组成：制约太阳风的起源

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摘要

The solar wind originates in the corona and hence is a direct sample of the solar atmosphere. In-situ observations of the solar wind elemental composition during approximately one solar cycle reveal important systematic variability of this composition, depending on solar wind regime and solar cycle. Recent observations of the solar atmosphere have also indicated that there is a rich variability of the elemental composition in the corona. For example, there are crucial fractionation processes between the spectroscopically determined photospheric composition and the coronal and solar wind compositions with a common feature. Elements with first ionization potential (FIP) less than ～10 eV are observed to be enhanced in the solar wind relative to the low-FIP elements. It is the purpose of this paper to quantify this variation for the solar wind and to relate the observed solar wind fractionation processes to the observed composition of the coronal plasma. We also address theoretical implications of these observations.
机译：太阳风起源于日冕，因此是太阳大气的直接样本。在大约一个太阳周期内对太阳风元素组成的原位观测表明，该组成的重要系统变异性取决于太阳风状况和太阳周期。最近对太阳大气的观察还表明，电晕中元素组成的变化很大。例如，在光谱确定的光球成分与具有共同特征的日冕和太阳风成分之间存在关键的分馏过程。观察到第一电离势（FIP）小于〜10 eV的元素在太阳风中相对于低FIP元素有所增强。本文的目的是量化太阳风的这种变化，并将观测到的太阳风分馏过程与观测到的日冕等离子体组成联系起来。我们还将讨论这些观察的理论含义。

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