Physics – Plasma Physics
Scientific paper
Jun 1985
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985esasp.235...37g&link_type=abstract
In ESA Future Missions in Solar, Heliospheric and Space Plasma Physics p 37-50 (SEE N86-27330 18-12)
Physics
Plasma Physics
6
Abundance, Chemical Composition, Ion Atom Interactions, Solar Corona, Solar Wind, Chromosphere, Electron States, Ionization Potentials, Particle Acceleration, Solar Temperature, Stellar Composition
Scientific paper
Measurements of abundances of elements and isotopes in the solar wind and their charge state distributions were used to study the corona and chromosphere. The composition and time variations of the solar wind indicate that two mechanisms are responsible for the observed differences between solar wind abundances and the composition in the outer convective zone of the Sun. The first mechanism is an atom-ion separation process, leading to an overabundance of elements with low first ionization potential in corona and solar wind. The second mechanism operates in the corona. Ions that are not well coupled to the protons and electrons by collisions or waves are not sufficiently accelerated to enter the solar wind with their full abundance. The anomalous abundances in the driver gas that follows flare driven interplanetary shocks imply that the corona (before perturbation) is compositionally stratified.
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