Computer Science
Scientific paper
Mar 1982
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982ssrv...33..201g&link_type=abstract
(Lindau Workshop on the Source Region of the Solar Wind, 9th, Lindau, West Germany, Nov. 1981.) Space Science Reviews, vol. 33,
Computer Science
102
Abundance, Cosmochemistry, Solar Corona, Solar Wind, Coronal Holes, Fractionation, Helium Isotopes, Hydrogen, Ionization
Scientific paper
Processes which may be capable of explaining the observed differences between solar wind abundances and abundances in the outer convective zone of the sun are examined. In a comparison of solar wind and outer convective zone compositions, it is shown that whereas the He/H ratio in the solar wind is highly variable and significantly lower than in the sun, heavier elements, including O, Si, Fe, Ne and Ar, are usually present at roughly solar levels. Processes which may account for this time-varying element and isotope fractionation in the solar wind include ion fractionation in the corona by mechanisms such as Coulomb friction, and processes occurring at lower solar altitudes, particularly ion-neutral separation in the chromosphere-transition zone. It is concluded that element and isotope fraction is probably the result of several mechanisms: coronal fractionation, producing the strong variability of He/H in low-speed solar wind; dynamic accumulation of He with subsequent ejection in flares; and separation dependent on incomplete ionization producing constant He depletion in high-speed streams.
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