Quasi-exospheric heat flux of solar-wind electrons

Details Quasi-exospheric heat flux of solar-wind electrons Quasi-exospheric heat flux of solar-wind electrons

May 1975

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1975aero.reptq....e&link_type=abstract

Interim Report Aerospace Corp., El Segundo, CA. Lab. Operations.

Physics

Exosphere, Heat Flux, Solar Electrons, Solar Wind, Electrostatic Charge, Magnetic Fields, Maxwell Equation, Plasma Oscillations, Potential Energy

Scientific paper

Density, bulk-velocity, and heat-flow moments are calculated for truncated Maxwellian distributions representing the cool and hot populations of solar-wind electrons, as realized at the base of a hypothetical exosphere. The electrostatic potential is thus calculated by requiring charge quasi-neutrality and the absence of electrical current. Plasma-kinetic coupling of the cool-electron and proton bulk velocities leads to an increase in the electrostatic potential and a decrease in the heat-flow moment.

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