Abstract
Recent papers have suggested that the slow solar wind is a super-position of material which is released by reconnection from large coronal loops. This reconnection process is driven by large-scale motions of solar magnetic flux driven by the non-radial expansion of the solar wind from the differentially rotating photosphere into more rigidly rotating coronal holes.
The elemental composition of the slow solar wind material is observed to be fractionated and more variable than the fast solar wind from coronal holes. Recently, it has also been reported that fractionation also occurs in 3He/4He. This may be interpreted in the frame-work of an existing model for fractionation on large coronal loops in which wave-particle interactions preferentially heat ions thereby modifying their scale-heights.
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Zurbuchen, T., Fisk, L., Gloeckler, G. et al. Element and Isotopic Fractionation in Closed Magnetic Structures. Space Science Reviews 85, 397–406 (1998). https://doi.org/10.1023/A:1005104030149
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DOI: https://doi.org/10.1023/A:1005104030149