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.
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