Abstract
Ionization-diffusion mechanisms to understand the first ionization potential (FIP) fractionation as observed in the solar corona and the solar wind are reviewed. The enrichment of the low-FIP elements (<10 eV) compared to the high-FIP elements, seen in e.g. slow and fast wind or polar plumes, is explained. The behaviour of the heavy noble gases becomes understandable. The absolute fractionation, i.e. in relation to hydrogen, can be calculated and fits well to the measurements. The theoretical velocity-dependence of the fractionation will with used to determine the velocities of the solar wind in the chromosphere.
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Peter, H. Element Separation in the Chromosphere Ionization-Diffusion Models for the FIP-Effect. Space Science Reviews 85, 253–260 (1998). https://doi.org/10.1023/A:1005150500590
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DOI: https://doi.org/10.1023/A:1005150500590