Analysis of O(7+)/O(6+) observations in the solar wind

Details Analysis of O(7+)/O(6+) observations in the solar wind Analysis of O(7+)/O(6+) observations in the solar wind

Oct 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985jgr....90.9881o&link_type=abstract

Journal of Geophysical Research (ISSN 0148-0227), vol. 90, Oct. 1, 1985, p. 9881-9884.

Astronomy and Astrophysics

Astronomy

8

Oxygen Ions, Solar Corona, Solar Temperature, Solar Wind Velocity, Electron Energy, International Sun Earth Explorers, Spaceborne Astronomy

Scientific paper

The ratio of O7+/O6+ in the solar wind can be used to deduce the temperature at the point in the corona where the charge states become "frozen" in the flow, and its determination therefore depends both upon the characteristics of the instrument and those of the source. The apparent increase of the ratio O7+/O6+ observed in the solar wind by K. W. Ogilvie and C. Vogt (1980) at speeds above 450 km s-1 has been reevaluated using a greatly expanded data set. The ratio observed for solar wind speeds less than 450 km s-1 corresponds to an electron temperature of 1.7±0.2×106K in the region of "freezing in" of the flow, as was previously reported. At higher speeds, when the kinetic temperature of the solar wind often exceeds 2 - 3×105K, instrumental effects become large and corrections difficult to determine.

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