A theoretical model for O5+ (O7+) ions in the fast solar wind

Details A theoretical model for O5+ (O7+) ions in the fast solar wind A theoretical model for O5+ (O7+) ions in the fast solar wind

Nov 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002jgra..107.1368c&link_type=abstract

Journal of Geophysical Research (Space Physics), Volume 107, Issue A11, pp. SSH 11-1, CiteID 1368, DOI 10.1029/2002JA009341

Physics

Plasma Physics

Interplanetary Physics: Solar Wind Plasma, Space Plasma Physics: Ionization Processes, Space Plasma Physics: Numerical Simulation Studies, Solar Physics, Astrophysics, And Astronomy: Coronal Holes, And Astronomy: General Or Miscellaneous

Scientific paper

We present a theoretical model for O5+ (O7+) ions as test particles in the fast solar wind using a previous turbulence-driven four-fluid model to establish the background solar wind, which consists of electrons, protons, alpha particles, and O6+ ions. The O5+ (O7+) ions in our model and the O6+ ions in the background are driven by the same mechanism, say, the resonant cyclotron interaction or an exponential heating addition. The ionization and recombination processes of O ions are taken into account. It is shown that the differential flow speeds between O6+ and O5+ or O7+, which are found to be in the range of 0.3-2, play very different roles in the formation of O charge states. This is due to discrepancy between the freezing-in distances of the two ion species. O7+ forms predominantly below 1.2 RS too close to the Sun to develop a differential streaming between O ions. O5+, on the other hand, freezes-in at about 1.8 RS where differential flows are well developed and therefore important for the formation of O5+ ions.

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