Magnetospheric convection at a low level power epsilon l

Details Magnetospheric convection at a low level power epsilon l Magnetospheric convection at a low level power epsilon l

Oct 1982

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982p%26ss...30.1057a&link_type=abstract

Planetary and Space Science, vol. 30, Oct. 1982, p. 1057-1059.

Physics

7

Convection, Dynamo Theory, Earth Magnetosphere, Solar Terrestrial Interactions, Solar Wind, Electron Energy, Magnetic Storms, Polar Caps

Scientific paper

It is demonstrated that the magnetospheric convection becomes evident in terms of the AE index only when the power epsilon of the solar wind-magnetosphere dynamo becomes greater than approximately 10 to the 18th ergs/sec or a slightly lower value. An enhanced conductivity is a crucial factor for the magnetospheric convection to manifest even in a low-level increase of the AE index of approximately 50-100 gamma.

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