What magnetospheric workers should know about solar wind composition

Details What magnetospheric workers should know about solar wind composition What magnetospheric workers should know about solar wind composition

Jan 1983

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983eice.conf...73b&link_type=abstract

IN: Energetic ion composition in the earth's magnetosphere (A84-37001 17-46). Tokyo/Dordrecht, Terra Scientific Publishing Co./D

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Heavy Ions, Magnetospheric Ion Density, Plasma Composition, Solar Terrestrial Interactions, Solar Wind, Abundance, Energy Spectra, Ion Probes, Ion Temperature, Isotopes, Proton Flux Density, Solar Corona

Scientific paper

The solar wind is a dynamic plasma flow which interacts with the magnetosphere through a variety of processes. Ions of the more common solar elements and isotopes are normally in the flow in various charge states, e.g., H-1(+), He-4(++), O(7+), O(6+), Si(9+)-Si(7+), and Fe(13+)-Fe(7+). These ions have abundances high enough that, in principle, they can be used for determining how the particles gain access to the magnetosphere, what fractions of the various ions enter, how they are accelerated and transported within the magnetosphere, and how they are ultimately lost. The present state of knowledge of the solar wind composition is reviewed, with emphasis on those features which might contribute to magnetospheric studies. The average elemental and isotopic abundances are given, along with a discussion of how they vary with time and with solar wind conditions. Two types of short-lived solar wind impulsive events which contain unusual ions are described. In one type, ions such as Fe(16+) and Si(12+) are found, and in the other, ions of He-4(+) and sometimes O(2+) and O(3+) are detected. The potential, as well as the limitations, of using solar wind composition as a test probe for magnetospheric studies are briefly considered.

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