Physics – Fluid Dynamics
Scientific paper
Nov 1983
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983nascp.2280.149o&link_type=abstract
In JPL Solar Wind Five p 149-162 (SEE N84-13067 03-92)
Physics
Fluid Dynamics
16
Electron Distribution, Fluid Dynamics, Heat Flux, Plasma Acceleration, Solar Wind, Interplanetary Magnetic Fields, Ion Density (Concentration), Ion Temperature, Solar Corona, Solar Electrons, Solar Flux
Scientific paper
The thermal and suprathermal processes involving solar wind electrons are discussed from a theoretical point of view. A model for the electron distribution function, f(e), based on the solutions of the Boltzmann equation in Krook's approximation is outlined: the angular and energy dependences of for various distances from the Sun between the coronal base and the Earth are presented with the express purpose of obtaining the radial profile of the heat flux generated by the suprathermals. The basic fluid-dynamical equations for the solar wind plasma as a whole along any given magnetic field line are solved. Results are in good agreement with observations. The predicted density and temperature profiles for positive ions exhibit the characteristics of recent measurements, both in the corona (above the coronal holes) and between 0.3 and 1 A.U. (the Helios region). It is concluded that the suprathermal electrons play an important role in the formation and the dynamics of the solar wind.
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