Solar control of the earth's emission of energetic O(+)

Details Solar control of the earth's emission of energetic O(+) Solar control of the earth's emission of energetic O(+)

Dec 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991jatp...53.1103l&link_type=abstract

(Solar-terrestrial physics; International SCOSTEP Symposium, 7th, The Hague, Netherlands, June 25-30, 1990, Selected Papers. A92

Physics

6

Current Sheets, Energetic Particles, Ion Emission, Oxygen Ions, Solar Terrestrial Interactions, Electromagnetic Acceleration, International Sun Earth Explorers, Interplanetary Magnetic Fields, Plasma-Particle Interactions, Solar Wind Velocity

Scientific paper

Energetic (0.1-16 keV/e) O(+) data obtained in the earth's plasma sheet (between 10 and 23 RE) by an ion mass spectrometer on the ISEE-1 spacecraft are compared statistically with published data on the concurrent solar wind and IMF. The most strongly variable parameter of the plasma sheet O(+) is its density, which is found to be well correlated with certain solar wind parameters, especially with the solar wind flow speed and the IMF component perpendicular to the flow vector. When those two solar wind parameters are combined to form an electric field (-v x B), both the number density and the energy density of the O(+) are found to vary in proportion to the square of that electric field, on average, suggesting that the emission of energetic O(+) ions from the earth may be powered by that same field. Based on this and on the previously published correlation with solar activity, it is argued that the emission of O(+) is controlled by a combination of HF (ionizing) and quasi-static (accelerating) solar electromagnetic fields.

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