Plasma sheet electromagnetic power generation and its dissipation along auroral field lines

Details Plasma sheet electromagnetic power generation and its dissipation along auroral field lines Plasma sheet electromagnetic power generation and its dissipation along auroral field lines

Aug 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002jgra..107.1181a&link_type=abstract

Journal of Geophysical Research (Space Physics), Volume 107, Issue A8, pp. SMP 14-1, CiteID 1181, DOI 10.1029/2001JA900136

Physics

17

Magnetospheric Physics: Magnetosphere/Ionosphere Interactions, Magnetospheric Physics: Plasma Waves And Instabilities, Magnetospheric Physics: Magnetospheric Configuration And Dynamics

Scientific paper

During a fortuitous meridional conjunction of Polar and Geotail at the nightside magnetosphere throughout the course of a geomagnetic substorm, measurements of Poynting flux indicate that most of the electromagnetic energy flux density that is radiated in the form of waves at the location of Geotail at ~18 RE is dissipated before it reaches Polar at ~5 RE, i.e., above the auroral acceleration region. While the Poynting flux measured at Polar (and to a greater extent at Geotail) is more than sufficient to account for particle acceleration below the satellite, it still represents a small portion of the earthward directed particle energy flux density measured at Geotail. If even a small portion of the bursty bulk flow energy couples to Alfven waves, it would be energetically sufficient to account for the expected auroral energy deposition during substorms. Power dissipation via kinetic Alfven waves along auroral field lines represents a viable mechanism by which localized reconnection flows can slow down. This may explain why fast earthward flows reported at midtail (>30 RE) distances can exist with no near-Earth counterpart and why any putative candidates of an ionospherically reflected flow burst pulse in the tail have very small amplitudes.

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