Observations of fluxes of suprathermal electrons accelerated by HF excited instabilities

Details Observations of fluxes of suprathermal electrons accelerated by HF excited instabilities Observations of fluxes of suprathermal electrons accelerated by HF excited instabilities

Dec 1982

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982jatp...44.1089c&link_type=abstract

(International Union of Radio Science, General Assembly on Ionospheric Modification, 20th, Washington, DC, Aug. 10-19, 1981.) Jo

Physics

Plasma Physics

52

Electron Acceleration, High Frequencies, Hot Electrons, Ionospheric Heating, Ionospheric Propagation, Magnetohydrodynamic Stability, Atmospheric Models, Electron Energy, Electronic Spectra, Flux (Rate), Plasma Physics, Plasma-Electromagnetic Interaction, Radio Transmitters

Scientific paper

During experiments at Arecibo transmitting about 140 kW of o-mode power at 7.63 MHz, which is near but below the foF2 (exciting strong plasma wave instabilities near an altitude of 285 km), nighttime plasma line intensities are found to be enhanced by a factor of 10-100. It is noted that these enhancements extend over a much broader altitude range than that to which HF excited plasma instabilities are confined. When the transmitter is turned off, these plasma line intensities immediately relax to their thermal level. Data which are seen as being helpful to future theoretical development are presented. One important conclusion is that electrons are accelerated up to at least 20 eV, an energy so high as to call for a reassessment of existing published theories. The data also contravene a highly sensitive HF power dependence of the suprathermal electron flux. The production rate is found to be relatively flat from 10 to 20 eV and relatively stable over several hours for constant HF power densities. Model calculations demonstrate that the observed altitude variation of the plasma line intensities is dominated by collisional energy degradation of the suprathermal electron flux to the neutral atmosphere and ionospheric plasma.

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