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

Jan 1976

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1976ap%26ss..39...65e&link_type=abstract

Astrophysics and Space Science, vol. 39, Jan. 1976, p. 65-73.

Astronomy and Astrophysics

Astrophysics

4

Exosphere, Heat Flux, Plasma Turbulence, Solar Electrons, Solar Wind, Coulomb Potential, Electron Distribution, Hot Electrons, Magnetohydrodynamic Stability, Velocity Distribution

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 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. If the velocities differ by the Alfven speed along the magnetic field, for example, the potential rises to 72.6 V and the heat flux falls to 0.0272 erg/sq cm per sec. In each case, the heat flux is carried mainly by the quasi-exospheric hot electrons.

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