Geoactive zones in the solar wind

Details Geoactive zones in the solar wind Geoactive zones in the solar wind

Apr 1975

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1975p%26ss...23..627b&link_type=abstract

Planetary and Space Science, vol. 23, Apr. 1975, p. 627-636.

Computer Science

1

Geomagnetism, Magnetic Storms, Proton Flux Density, Satellite Observation, Solar Wind Velocity, Explorer 33 Satellite, Interplanetary Magnetic Fields, Plasma Diagnostics, Solar Eclipses, Solar Protons, Solar Wind

Scientific paper

A reassessment of geoactive parameters is undertaken. It finds three parameters to be geoactive: proton number density n, the Z-component of the frozen-in magnetic field in solar ecliptic coordinates, and magnetic field variability delta-B. Since a corpuscular stream differs from the quiet solar wind only in higher bulk velocity v, and since v is not a geoactive parameter, corpuscular streams are not more geoactive than the quiet solar wind. The concept of geoactive zones, characterized by the enhancement of some geoactive parameter, is reviewed and applied to an analysis of the geomagnetic storm of July 8-10, 1966.

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