Helium and minor ions in the corona and solar wind - Dynamics and charge states

Details Helium and minor ions in the corona and solar wind - Dynamics and charge states Helium and minor ions in the corona and solar wind - Dynamics and charge states

Feb 1986

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986soph..103..347b&link_type=abstract

Solar Physics (ISSN 0038-0938), vol. 103, no. 2, 1986, p. 347-383. SNSF-supported research.

Physics

95

Helium Ions, Ion Charge, Ion Concentration, Solar Corona, Solar Wind, Abundance, Electron Density (Concentration), Magnesium, Oxygen Ions, Silicon, Solar Protons, Solar Wind Velocity, Two Fluid Models

Scientific paper

A theoretical model of the acceleration region of the solar wind with major species (p, alpha, e) and minor ions (e.g., He-3, C, O, Mg, Si) is presented. Observed n(e)-profiles and the equations of continuity and momentum are used to calculate profiles of T, n, and u for all species, as well as charge states of minor ions. The disagreement of the results of a pure p-e model with observations is discussed in some detail, and it is shown that a model consistent with observations both in the corona and at 1 AU requires a finite abundance of He(2+). This model predicts a strong enhancement of He/H in the lower corona. The results for the frozen-in charge states in the p-alpha-e model are in agreement with measurements in the low speed solar wind, especially for the well determined pair O(6+)/O(7+). Finally, a model for a coronal hole is investigated and it is found that wave pressure is necessary to model successfully the observed solar wind speeds and abundances. Although various simplifying assumptions had to be introduced, care was taken to ensure that the model remains physically consistent, i.e., that the same physics is used for the major species as well as the minor ions.

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