Power dissipation at slow-mode shocks in the distant geomagnetic tail

Details Power dissipation at slow-mode shocks in the distant geomagnetic tail Power dissipation at slow-mode shocks in the distant geomagnetic tail

Oct 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984georl..11.1058f&link_type=abstract

Geophysical Research Letters (ISSN 0094-8276), vol. 11, Oct. 1984, p. 1058-1061. Research sponsored by the U.S. Department of En

Physics

22

Energy Dissipation, Geomagnetic Tail, Magnetospheric Instability, Poynting Theorem, Shock Wave Propagation, Solar Terrestrial Interactions, Electric Field Strength, International Sun Earth Explorers, Magnetic Flux, Magnetic Storms, Magnetohydrodynamic Waves, Magnetospheric Electron Density, Space Plasmas

Scientific paper

An estimate is made of the decreases in Poynting flux across slow shocks in the geomagnetic tail detected by the ISEE-3 spacecraft. An electron analyzer and a magnetometer recorded 26 of the events in January-February 1983. Two-dimensional electron velocity distributions parallel to the magnetic field across the shock transition characterized the data. The shocks were of relatively high strength, close to the switch-off limit, and displayed a large upstream Alfven Mach number. The Poynting flux decreased an average of 0.0018-0.0166 ergs/sq cm per sec. The power dissipated from lobe-magnetic energy density to plasma sheet convection across the shocks is estimated to be 5 x 10 to the 18th ergs/sec.

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