Rate of magnetic-flux accumulation in the magnetospheric tail

Details Rate of magnetic-flux accumulation in the magnetospheric tail Rate of magnetic-flux accumulation in the magnetospheric tail

Jun 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985ge%26ae..25..458r&link_type=abstract

Geomagnetizm i Aeronomiia (ISSN 0016-7940), vol. 25, May-June 1985, p. 458-463. In Russian.

Computer Science

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2

Geomagnetic Tail, Interplanetary Magnetic Fields, Magnetic Flux, Magnetospheric Instability, Plasma Layers, Magnetic Storms, Satellite Sounding, Solar Wind

Scientific paper

Satellite (OGO-5 and HEOS-1) data are used to obtain quantitative results concerning the dependence of the rate of magnetic-flux accumulation in the magnetospheric tail on the parameters of the interplanetary medium during preliminary substorm phases as well as in the case of stationary external conditions. It is concluded that the accumulated flux is due to reconnection processes in the daytime sector, and that the electric field in the plasma sheet of the tail is significantly attenuated during these periods.

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