Auroral energy input from energetic electrons and Joule heating at Chatanika

Details Auroral energy input from energetic electrons and Joule heating at Chatanika Auroral energy input from energetic electrons and Joule heating at Chatanika

Nov 1975

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1975jgr....80.4364w&link_type=abstract

Journal of Geophysical Research, vol. 80, Nov. 1, 1975, p. 4364-4367. NSF-supported research;

Computer Science

Sound

5

Auroras, Electron Precipitation, High Energy Electrons, Ionospheric Heating, Radar Measurement, E Region, Ionospheric Sounding, Ohmic Dissipation, Photometry, Recombination Coefficient, Resistance Heating

Scientific paper

A procedure is examined whereby the incident energy flux of auroral electrons is ascertained from radar measurements. Radar-determined fluxes are compared with those ascertained from simultaneous photometric observations at 4278 A. The fluxes obtained by both techniques had similar magnitudes and time variations. If one assumes that the largest uncertainty in the radar/photometer comparison is the effective recombination coefficient, then that coefficient can also be deduced. A value of 3 times 10 to the minus seventh cu cm per sec is found at about 105 km, which is in good agreement with other recent determinations during active auroral conditions. This technique is then combined with another to ascertain the Joule heating in order to determine the energy input from the magnetosphere to the ionosphere in a region localized above the radar in the midnight sector. The energy input is continuous at a significant level, i.e., greater than the 3 ergs/sq cm s that could be delivered by the sun, were it overhead. Moreover, at times, each of these inputs became as great as 30 ergs/sq cm s.-

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